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 503

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	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
2	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
3	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
4	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
5	SS 433	287.9527	4.99	287.334904	4.905608	290.182673	27.181461	39.69879316	-2.23786427	78.6446	53833.4611458333	2006-04-08 11:04:03	53834.4579166667	2006-04-09 10:59:24	401004010	40.1976	40	40.2216	40.1976	40.2296	40.2136	2	2	2	2	1	0	0	30.4749	30.4749	86.11	2	PROCESSED	57533.4357638889	2016-05-25 10:27:30	54400	2007-10-27 00:00:00	53906.5501736111	2006-06-20 13:12:15	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010031	SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber.	GALACTIC POINT SOURCES	4	A	NOBUYUKI KAWAI		JAP	1	AO1	SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401004010/	Quick Look
6	1E1207.4-5209	182.4916	-52.442	181.83735	-52.163724	209.144209	-45.784625	296.53791481	9.91413144	148.6893	54146.2087384259	2007-02-15 05:00:35	54147.6390509259	2007-02-16 15:20:14	401030020	49.8266	50	50.0734	49.8266	0	50.0894	1	2	0	1	1	0	0	44.4468	44.4468	123.576	2	PROCESSED	57537.4372337963	2016-05-29 10:29:37	54750	2008-10-11 00:00:00	54153.9886458333	2007-02-22 23:43:39	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010152	1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object.	GALACTIC POINT SOURCES	4	B	ATSUMASA YOSHIDA		JAP	1	AO1	A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401030020/	Quick Look
7	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
8	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
9	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
10	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
11	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
12	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
13	V1223 SGR	283.7445	-31.105	282.940068	-31.169256	281.851865	-8.228404	5.0082738	-14.31987205	79.9528	54203.4803240741	2007-04-13 11:31:40	54204.9418055556	2007-04-14 22:36:12	402002010	60.706	60	60.706	60.706	0	60.706	2	2	0	2	1	0	0	46.2861	46.2861	126.2719	2	PROCESSED	57538.1822800926	2016-05-30 04:22:29	54744	2008-10-05 00:00:00	54210.6596875	2007-04-20 15:49:57	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020008	The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS.	GALACTIC POINT SOURCES	4	A	MANABU ISHIDA		JAP	2	AO2	MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402002010/	Quick Look
14	PSR B1259-63	195.6556	-63.8839	194.86632	-63.61523	227.712317	-50.941906	304.16255435	-1.03887935	293.4832	54304.2811226852	2007-07-23 06:44:49	54304.6877777778	2007-07-23 16:30:24	402014050	19.7023	20	19.7023	19.7023	0	19.7023	1	1	0	1	1	0	0	17.7549	17.7549	35.1279	0	PROCESSED	57539.3024768518	2016-05-31 07:15:34	54707	2008-08-29 00:00:00	54339.2175347222	2007-08-27 05:13:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014050/	Quick Look
15	LS 5039	276.5633	-14.9109	275.848755	-14.941003	276.400444	8.383997	16.82651822	-1.31880921	270.412	54352.6780555556	2007-09-09 16:16:24	54358.4725	2007-09-15 11:20:24	402015010	203.2399	200	203.2399	203.2399	0	203.2399	2	2	0	2	1	0	0	181.095	181.095	442.0879	4	PROCESSED	57540.0947685185	2016-06-01 02:16:28	54745	2008-10-06 00:00:00	54384.7259027778	2007-10-11 17:25:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020062	The periodicity of TeV gamma-rays from the Galactic microquasar LS 5039 has recently been detected by the HESS Cherenkov telescope. We propose to conduct a simultaneous X-ray/VHE gamma-ray observations for a total of 200 ks of the microquasar with Suzaku XIS and HXD in conjuction with the HESS telescope. A full orbital period of 3.9 days is planned to be covered with Suzaku and HESS. The goal of this program is to study a possible correlation of X-TeV fluxes and spectral changes as a function of orbital phase, thereby shedding a new light on the origin of high-energy radiation from the microquasar system.	GALACTIC POINT SOURCES	4	A	TADAYUKI TAKAHASHI		JAP	2	AO2	SIMULTANEOUS SUZAKU AND HESS OBSERVATIONS OF THE TEV GAMMA-RAY MICROQUASAR LS 5039	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402015010/	Quick Look
16	4U 1700+24	256.6316	23.9071	256.110961	23.972677	252.098688	46.519124	45.07419011	32.98144858	280.149	54334.7787615741	2007-08-22 18:41:25	54335.875162037	2007-08-23 21:00:14	402023010	50.2445	50	50.2525	50.2605	0	50.2445	2	2	0	2	1	0	0	45.3268	45.3268	94.7158	2	PROCESSED	57539.6636226852	2016-05-31 15:55:37	54723	2008-09-14 00:00:00	54350.4606481482	2007-09-07 11:03:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020105	We propose the observation of Neutron Star Low Mass X-ray Binary (LMXB) system 4U 1700+24.This system would be Advection Dominant Accretion Flow (ADAF) and we research the hard-tail in hard X-ray region. Though the X-ray intensity in a Low Hard state is very faint, $sim$10$^{33}$ erg/s we can obtain the energy spectrum of 10-100keV for the first time using Suzaku 50ksec observation because it is the nearest LMXB. If we know the extension of hard-tail in low luminosity state, we can understand the physical state of electron in the accretion disk and/or compact object. Suzaku is the best satellite to research the faint emission around 100keV.	GALACTIC POINT SOURCES	4	B	OSAMU NAGAE		JAP	2	AO2	STUDY OF MASS ACCRETION FLOW IN ADAF FOR LOW LUMINOUS X-RAY BINARY 4U 1700+24	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402023010/	Quick Look
17	CYG OB2 ASSOCIATION	308.2175	41.2935	307.768848	41.122144	329.008943	57.17316	80.16491027	0.83267098	220.3949	54452.9185532407	2007-12-18 22:02:43	54453.843912037	2007-12-19 20:15:14	402030010	41.1147	40	41.1147	41.1147	0	41.1147	2	2	0	2	1	0	0	37.9181	37.9181	79.9439	0	PROCESSED	57540.9006597222	2016-06-01 21:36:57	54828	2008-12-28 00:00:00	54460.6521643518	2007-12-26 15:39:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020150	Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku.	GALACTIC POINT SOURCES	4	C	SHUNJI KITAMOTO		JAP	2	AO2	STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402030010/	Quick Look
18	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
19	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
20	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
21	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
22	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
23	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
24	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
25	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
26	1E 1048.1-5937	162.5452	-59.8394	162.049535	-59.57411	203.219635	-58.558248	288.24102095	-0.47209541	101.4368	54800.9597337963	2008-11-30 23:02:01	54802.5927083333	2008-12-02 14:13:30	403005010	100.4231	100	100.443	100.4231	0	100.4231	2	2	0	2	1	0	0	68.1049	68.1049	141.0819	0	PROCESSED	57544.6078472222	2016-06-05 14:35:18	55178	2009-12-13 00:00:00	54812.0471875	2008-12-12 01:07:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030013	Observations in soft X-ray through hard X-ray bands are key to understand the emission processes in the magnetosphere of Anomalous X-ray Pulsars (AXPs). We propose to observe the two AXPs, 1E 2259+586 and 1E 1048.1-5937, with SUZAKU. Although no detections of the hard X-ray emissions have been reported, the results of the simulation using XSPEC for HXD indicate that SUZAKU detects the hard X-ray emissions above 20~keV from both AXPs for the first time with a quite high probability. The time resolution of HXD is able to provide the pulse profiles and the phase-resolved spectra in hard X-rays emissions. With these results of the observations, SUZAKU will provide a crucial information to study the emission processes in the magnetosphere of AXPs.	GALACTIC POINT SOURCES	4	C	JUMPEI TAKATA		JAP	3	AO3	X-RAY OBSERVATIONS OF ANOMALOUS X-RAY PULSARS WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403005010/	Quick Look
27	MARS-P3	102.9612	25.1565	102.192848	25.217116	101.724463	2.241555	190.28784034	11.26022306	298.032	54559.4933796296	2008-04-03 11:50:28	54559.5766087963	2008-04-03 13:50:19	403006030	3.886	100	3.886	3.91	0	3.894	1	1	0	1	1	0	0	3.1134	3.1134	7.1839	0	PROCESSED	57542.0373148148	2016-06-03 00:53:44	54953	2009-05-02 00:00:00	54577.0484259259	2008-04-21 01:09:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006030/	Quick Look
28	MARS-P11	103.2936	25.1207	102.525618	25.182892	102.027614	2.233108	190.44969799	11.5184009	298.1493	54560.1601041667	2008-04-04 03:50:33	54560.2433333333	2008-04-04 05:50:24	403006110	4.6198	100	4.6278	4.6198	0	4.6358	1	1	0	1	1	0	0	4.0749	4.0749	7.1839	0	PROCESSED	57542.0559490741	2016-06-03 01:20:34	54953	2009-05-02 00:00:00	54577.1745023148	2008-04-21 04:11:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006110/	Quick Look
29	MARS-P13	103.3779	25.1101	102.610021	25.172691	102.104653	2.229561	190.49210676	11.58330245	298.1799	54560.3267708333	2008-04-04 07:50:33	54560.41	2008-04-04 09:50:24	403006130	4.2518	100	4.2678	4.2518	0	4.2678	1	1	0	1	1	0	0	3.529	3.529	7.1839	0	PROCESSED	57542.0605671296	2016-06-03 01:27:13	54953	2009-05-02 00:00:00	54577.9292939815	2008-04-21 22:18:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006130/	Quick Look
30	MARS-P16	103.503	25.0968	102.735261	25.159983	102.218767	2.2268	190.55275085	11.68067717	298.2223	54560.5768171296	2008-04-04 13:50:37	54560.66	2008-04-04 15:50:24	403006160	2.3262	100	2.3262	2.3262	0	2.3262	2	2	0	2	1	0	0	2.134	2.134	7.1799	0	PROCESSED	57542.0664236111	2016-06-03 01:35:39	54953	2009-05-02 00:00:00	54577.9478935185	2008-04-21 22:44:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006160/	Quick Look
31	MARS-P21	103.7101	25.0688	102.942627	25.132964	102.408276	2.21649	190.65860601	11.8395058	298.2947	54560.9933217593	2008-04-04 23:50:23	54561.0765509259	2008-04-05 01:50:14	403006210	2.8808	100	2.8808	2.8808	0	2.8808	1	1	0	1	1	0	0	3.4516	3.4516	7.1839	0	PROCESSED	57542.0774884259	2016-06-03 01:51:35	54953	2009-05-02 00:00:00	54578.0612847222	2008-04-22 01:28:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006210/	Quick Look
32	MARS-P23	103.7955	25.0599	103.028122	25.124467	102.486187	2.214951	190.69976585	11.90614711	298.325	54561.1600347222	2008-04-05 03:50:27	54561.2432175926	2008-04-05 05:50:14	403006230	4.5188	100	4.5268	4.5188	0	4.5348	1	1	0	1	1	0	0	3.6868	3.6868	7.1839	0	PROCESSED	57542.0791898148	2016-06-03 01:54:02	54953	2009-05-02 00:00:00	54578.1176157407	2008-04-22 02:49:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006230/	Quick Look
33	MARS-P25	103.8803	25.0503	103.113021	25.115268	102.56363	2.212708	190.74132534	11.97202775	298.3546	54561.3266550926	2008-04-05 07:50:23	54561.4098842593	2008-04-05 09:50:14	403006250	4.2612	100	4.2692	4.2612	0	4.2692	1	1	0	1	1	0	0	3.2511	3.2511	7.1839	0	PROCESSED	57542.2336458333	2016-06-03 05:36:27	54953	2009-05-02 00:00:00	54578.1323032407	2008-04-22 03:10:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006250/	Quick Look
34	MARS-P26	103.921	25.0474	103.153759	25.112561	102.600638	2.213348	190.75967691	12.00436516	298.3671	54561.4100347222	2008-04-05 09:50:27	54561.4932175926	2008-04-05 11:50:14	403006260	4.7976	100	4.8136	4.7976	0	4.8216	1	1	0	1	1	0	0	3.7622	3.7622	7.1839	0	PROCESSED	57542.2337962963	2016-06-03 05:36:40	54953	2009-05-02 00:00:00	54578.1374074074	2008-04-22 03:17:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006260/	Quick Look
35	ARCHES CLUSTER	266.4808	-28.778	265.687528	-28.758983	266.892731	-5.374834	0.16960578	0.02569084	109.9998	54911.0857407407	2009-03-21 02:03:28	54913.7681712963	2009-03-23 18:26:10	403009010	110.7933	100	110.7933	110.7933	0	110.7933	2	2	0	2	1	0	0	91.6578	91.6578	231.7417	3	PROCESSED	57545.9555787037	2016-06-06 22:56:02	55330	2010-05-14 00:00:00	54924.3822106482	2009-04-03 09:10:23	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030029	We propose to observe a hard X-ray ring which has an emission line around 6.4 keV, located at the north of the Arches cluster. The ring is probably produced by an energetic jet or a supernova explosion. We aim to determine the continuum shape, the center energy of the emission line, and the absorption column to figure out the origin of the ring.	GALACTIC POINT SOURCES	4	B	MASAHIRO TSUJIMOTO		JAP	3	AO3	A 6.4 KEV RING AT THE NORTH OF THE ARCHES CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403009010/	Quick Look
36	LS I+61 303_1	40.1455	61.188	39.183267	60.973753	59.828193	42.868734	135.69810374	1.0510579	270.0003	54853.9515856482	2009-01-22 22:50:17	54854.8648032407	2009-01-23 20:45:19	403015010	40.5514	40	40.5514	40.5514	0	40.5514	2	2	0	2	1	0	0	25.7312	25.7312	78.868	0	PROCESSED	57545.3022916667	2016-06-06 07:15:18	55329	2010-05-13 00:00:00	54880.5343865741	2009-02-18 12:49:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030077	We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST.	GALACTIC POINT SOURCES	4	A	YASUSHI FUKAZAWA		JAP	3	AO3	X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403015010/	Quick Look
37	LS I+61 303_2	40.1457	61.1877	39.18347	60.973453	59.828143	42.868421	135.69831419	1.05082335	270.0006	54856.6966087963	2009-01-25 16:43:07	54858.1766666667	2009-01-27 04:14:24	403016010	61.0667	60	61.0784	61.0667	0	61.0784	2	2	0	2	1	0	0	26.6591	26.6591	127.8398	1	PROCESSED	57545.3828819444	2016-06-06 09:11:21	55329	2010-05-13 00:00:00	54880.5522106482	2009-02-18 13:15:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030077	We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST.	GALACTIC POINT SOURCES	4	A	YASUSHI FUKAZAWA		JAP	3	AO3	X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403016010/	Quick Look
38	LS I+61 303_3	40.2018	61.1949	39.239095	60.980826	59.865781	42.86376	135.72005286	1.06843757	246.2753	54872.1842592593	2009-02-10 04:25:20	54873.7252199074	2009-02-11 17:24:19	403017010	68.6273	60	68.6273	68.6273	0	68.6273	2	2	0	2	1	0	0	65.0685	65.0685	133.1218	1	PROCESSED	57545.5290856482	2016-06-06 12:41:53	55330	2010-05-14 00:00:00	54893.4210300926	2009-03-03 10:06:17	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030077	We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST.	GALACTIC POINT SOURCES	4	A	YASUSHI FUKAZAWA		JAP	3	AO3	X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403017010/	Quick Look
39	IGR J16194-2810	244.8908	-28.0663	244.116394	-27.946439	247.849887	-6.534784	349.1669856	15.58223604	95.1879	54867.1762152778	2009-02-05 04:13:45	54868.4314236111	2009-02-06 10:21:15	403024010	45.5687	50	45.5687	45.5738	0	45.5687	2	2	0	2	1	0	0	38.7859	38.7859	108.4358	1	PROCESSED	57545.4895023148	2016-06-06 11:44:53	55329	2010-05-13 00:00:00	54880.5743518518	2009-02-18 13:47:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030121	We propose to observe the weakly magnetized neutron star X-ray binary, IGR J16194-2810. This target object has almost constant luminosity and is expected to be state of ADAF. Assuming that we observe the object using HXD and XIS of the Suzaku for 50ks, we can investigate the soft X-ray emission from the NS and/or the accretion disk and hard X-ray tail. Comparing Black Body and Disk Black Body parameters of this object with that of fainter source, 4U 1700+24, we obtain a picture of accretion disk and accretion flow. If we measure the photon index and cutoff energy of the hard tail, we can reveal the physical condition of corona surrounding the NS or the disk. Only Suzaku can carry out this observation which observe soft-thermal and hard-nonthermal X-ray emission from faint source.	GALACTIC POINT SOURCES	4	C	OSAMU NAGAE		JAP	3	AO3	ELUCIDATION OF THE ADAF OBSERVING LOW LUMINOUS NEUTRON STAR X-RAY BINARY IGR J16194-2810	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403024010/	Quick Look
40	V709 CAS	7.1951	59.3013	6.498819	59.024957	38.349683	49.774418	120.03837674	-3.44309479	84.0816	54637.4334837963	2008-06-20 10:24:13	54638.1542824074	2008-06-21 03:42:10	403025010	35.8982	30	35.8982	35.8982	0	35.8982	2	2	0	2	1	0	0	33.3823	33.3823	62.2679	0	PROCESSED	57542.8811921296	2016-06-03 21:08:55	55014	2009-07-02 00:00:00	54648.3358101852	2008-07-01 08:03:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030140	Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	3	AO3	IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403025010/	Quick Look
41	RX J1940.1-1025	295.0445	-10.4193	294.356962	-10.535652	295.074294	10.867465	28.98688715	-15.49869645	79.7405	54572.8979976852	2008-04-16 21:33:07	54573.743275463	2008-04-17 17:50:19	403027010	32.4536	30	32.4536	32.4536	0	32.4536	2	2	0	2	1	0	0	26.4657	26.4657	73.0219	2	PROCESSED	57542.3241087963	2016-06-03 07:46:43	54953	2009-05-02 00:00:00	54587.0481481482	2008-05-01 01:09:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030140	Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	3	AO3	IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403027010/	Quick Look
42	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
43	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
44	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
45	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
46	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
47	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
48	GS 1826-238	277.3735	-23.8572	276.610421	-23.891095	276.73109	-0.588705	9.22092987	-6.12003001	267.2862	55125.8488310185	2009-10-21 20:22:19	55127.9502777778	2009-10-23 22:48:24	404007010	102.5154	100	102.5154	102.5314	0	102.5372	2	2	0	2	1	0	0	87.9996	87.9996	181.5418	2	PROCESSED	57549.0104976852	2016-06-10 00:15:07	55534	2010-12-04 00:00:00	55166.4220833333	2009-12-01 10:07:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040035	We propose a 100 ksec Suzaku observation of the neutron star (NS) binary GS 1826-238. It is already known that there is a high energy cutoff at around 150 keV in the hard state of black hole candidates (BNCs). Additional non-thermal spectrum above 300 keV has sometimes been verified by gamma-ray observatories. Some NS binaries exhibit a 'hard state' which shows X-ray properties similar to those observed in hard state BHCs. Their cutoff energies (~50 keV) are systematically lower than those of BHCs, but firm detections of non-thermal emissions are not reported so far. This proposal is aimed at the first detection of the non-thermal hard tail from this source in the steady 'hard state', and verification of its possible jet origin via simultaneous radio, near-IR, and optical observations.	GALACTIC POINT SOURCES	4	B	KAZUTAKA YAMAOKA		JAP	4	AO4	SEARCH FOR A NON-THERMAL HARD TAIL FROM THE NEUTRON STAR BINARY GS 1826-238	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404007010/	Quick Look
49	EUVE J0317-85.5	48.9864	-85.5003	51.11405	-85.679196	278.533864	-69.749958	299.84736337	-30.72881529	65.46	55028.6017476852	2009-07-16 14:26:31	55030.1460185185	2009-07-18 03:30:16	404019010	63.0843	60	63.0843	63.0843	0	63.0843	2	2	0	2	1	0	0	56.8965	56.8965	133.4138	1	PROCESSED	57547.8712847222	2016-06-08 20:54:39	55406	2010-07-29 00:00:00	55040.2674305556	2009-07-28 06:25:06	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040083	Where is the particle acceleration site in the universe? The Cosmic-ray origin is the long standing mystery for near 100 years. The first discovery of "the white dwarf pulsar" in the AE Aquarii system with Suzaku is one of the most important step in this study, because Suzaku demonstrated the possibility of particle acceleration in white dwarfs. The next important step is to search for the sign of non-thermal emission from a NORMAL white dwarf. Here, we propose the Suzaku observation of an isolated white dwarf EUVE J0317-85.5, which has very high magnetic field strength of 450 MG and very fast rotation period 725 sec among this type of objects.	GALACTIC POINT SOURCES	4	B	ATSUSHI HARAYAMA		JAP	4	AO4	FIRST SEARCH FOR NON THERMAL EMISSION FROM AN ISOLATED MAGNETIZED WHITE DWARF	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404019010/	Quick Look
50	TT ARI	31.7181	15.2972	31.038138	15.059527	34.795947	2.311089	148.52228749	-43.79443	71.0668	55018.4424652778	2009-07-06 10:37:09	55019.3023611111	2009-07-07 07:15:24	404021010	35.7421	35	35.7421	35.7796	0	35.7876	2	2	0	2	1	0	0	31.794	31.794	74.2578	1	PROCESSED	57547.7822453704	2016-06-08 18:46:26	55399	2010-07-22 00:00:00	55029.236712963	2009-07-17 05:40:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040095	The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail.	GALACTIC POINT SOURCES	4	B	KEI SAITOU		JAP	4	AO4	IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404021010/	Quick Look
51	TX COL	85.7822	-41.0648	85.383592	-41.086265	82.635964	-64.399356	246.79781267	-29.77494364	322.4827	54963.6800578704	2009-05-12 16:19:17	54965.2502199074	2009-05-14 06:00:19	404031010	59.7818	40	59.7898	59.7898	0	59.7818	2	2	0	2	1	0	0	51.123	51.123	135.654	0	PROCESSED	57546.5734143518	2016-06-07 13:45:43	55345	2010-05-29 00:00:00	54978.2105439815	2009-05-27 05:03:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040113	We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.	GALACTIC POINT SOURCES	4	A	TAKAYUKI YUASA		JAP	4	AO4	SURVEY OBSERVATION OF INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404031010/	Quick Look
52	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
53	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
54	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
55	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
56	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
57	4U 1820-30	275.9251	-30.4172	275.121541	-30.443999	275.136917	-7.082068	2.74021083	-7.94370371	265.2009	55111.1096643518	2009-10-07 02:37:55	55111.700162037	2009-10-07 16:48:14	404069050	21.7674	20	21.7674	21.7674	0	21.7674	1	1	0	1	1	0	0	15.6743	15.6743	51.0039	0	PROCESSED	57548.7799884259	2016-06-09 18:43:11	55496	2010-10-27 00:00:00	55127.2938194445	2009-10-23 07:03:06	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069050/	Quick Look
58	GX 9+9	262.9404	-16.8929	262.215892	-16.856936	263.194726	6.381396	8.57505694	9.06920034	97.5329	55271.6738773148	2010-03-16 16:10:23	55273.9918981482	2010-03-18 23:48:20	404071010	85.1871	75	85.2087	85.2031	0	85.1871	2	1	0	2	1	0	0	61.6942	61.6942	200.2639	0	PROCESSED	57550.9767476852	2016-06-11 23:26:31	55652	2011-04-01 00:00:00	55285.4179513889	2010-03-30 10:01:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042011	We propose two 75 ks Suzaku observations of the bright neutron star low mass X-ray binary (LMXB) GX9+9, spread over six months. We will investigate the presence of X-ray narrow absorption features in the Suzaku spectra, which are a signature of a disk wind. Such features, identified with ions such as Fe XXV and Fe XXVI, have been observed in a number of LMXBs and give us information about the mass outflow rate and the launching mechanism of the wind. We will study the connection of the disk wind to the presence of radio jet emission with simultaneous radio observations. Finally, we will determine if the broad Fe emission line indicated by the XMM-Newton spectrum is relativistically broadened. Variability will be studied as a function of accretion rate in the two proposed observations.	GALACTIC POINT SOURCES	4	B	MARIA DIAZ TRIGO		EUR	4	AO4	A STUDY OF THE DISK WIND-JET CONNECTION IN GX9+9 WITH MULTIWAVELENGTH OBSERVATIONS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404071010/	Quick Look
59	CYGNUS X-1	299.5392	35.2589	299.069624	35.122644	313.628523	54.317489	71.36219421	3.13231837	55.3254	54957.7006828704	2009-05-06 16:48:59	54958.1356365741	2009-05-07 03:15:19	404075060	19.4345	300	19.4345	19.4505	0	19.4345	2	1	0	2	1	0	0	15.2795	15.2795	37.5579	0	PROCESSED	57546.5121412037	2016-06-07 12:17:29	54922	2009-04-01 00:00:00	54976.0885300926	2009-05-25 02:07:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075060/	Quick Look
60	CYGNUS X-1	299.5373	35.2573	299.067717	35.121052	313.625096	54.316504	71.3600172	3.13281014	53.4895	54976.3582060185	2009-05-25 08:35:49	54976.8259722222	2009-05-25 19:49:24	404075090	20.9252	300	20.9252	20.9332	0	20.9252	2	1	0	2	1	0	0	16.1164	16.1164	40.412	1	PROCESSED	57546.6796296296	2016-06-07 16:18:40	54922	2009-04-01 00:00:00	54992.6651736111	2009-06-10 15:57:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075090/	Quick Look
61	CYGNUS X-1	299.5294	35.2515	299.059794	35.115286	313.611339	54.313209	71.35169447	3.13529932	46.7675	54984.481400463	2009-06-02 11:33:13	54984.9870833333	2009-06-02 23:41:24	404075110	17.4502	300	19.037	17.7782	0	17.4502	1	1	0	1	1	0	0	15.0409	15.0409	43.6879	1	PROCESSED	57547.4475462963	2016-06-08 10:44:28	54922	2009-04-01 00:00:00	54994.4091087963	2009-06-12 09:49:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075110/	Quick Look
62	CYGNUS X-1	299.6354	35.1397	299.164908	35.003038	313.686688	54.178801	71.30132058	3.00311627	241.1557	55159.514224537	2009-11-24 12:20:29	55160.1328587963	2009-11-25 03:11:19	404075180	21.7685	300	21.7685	22.4805	0	22.4725	5	2	0	3	1	0	0	11.4064	11.4064	53.4358	0	PROCESSED	57549.5783680556	2016-06-10 13:52:51	54922	2009-04-01 00:00:00	55176.294849537	2009-12-11 07:04:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075180/	Quick Look
63	4U0142+61	26.5176	61.8112	25.649771	61.561225	52.160955	46.451759	129.33625727	-0.37933599	61.041	55055.0703125	2009-08-12 01:41:15	55057.3654976852	2009-08-14 08:46:19	404079010	107.4129	100	107.4129	107.4209	0	107.4227	2	2	0	2	1	0	0	99.7576	99.7576	198.2838	2	PROCESSED	57548.2012152778	2016-06-09 04:49:45	54922	2009-04-01 00:00:00	55068.3037268518	2009-08-25 07:17:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	4	AO4	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404079010/	Quick Look
64	PSR J1846-0258	281.5972	-2.9106	280.942424	-2.965017	282.329422	20.034924	29.7662115	-0.20474108	86.0001	54936.8175578704	2009-04-15 19:37:17	54939.6779398148	2009-04-18 16:16:14	404081010	104.3451	100	104.3451	104.3675	0	104.3531	2	2	0	2	1	0	0	76.0065	76.0065	247.1018	1	PROCESSED	57546.2746990741	2016-06-07 06:35:34	54922	2009-04-01 00:00:00	54959.5006018518	2009-05-08 12:00:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	4	AO4	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404081010/	Quick Look
65	V773TAU	63.5571	28.1952	62.783682	28.069565	66.716115	6.867305	168.22500409	-16.34364304	260.6557	55610.1581712963	2011-02-18 03:47:46	55611.9815277778	2011-02-19 23:33:24	405011010	82.2463	80	82.2543	82.2463	0	82.2543	2	2	0	2	1	0	0	72.8287	72.8287	157.5258	2	PROCESSED	57601.0256134259	2016-08-01 00:36:53	55990	2012-03-04 00:00:00	55621.2978703704	2011-03-01 07:08:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050033	We propose a Suzaku observation of the pre-main sequence binary system V773 Tau with the high sensitivity of HXD. The empirical Lx-Lr relation (Benz-G"udel relation) and radio flux variation predict that this source can have a flare with a peak luminosity Lx=10^34 ergs s-1, seven orders of magnitude larger than that of the Sun, when it is just before the periastron passage. We will observe this target simultaneously with radio band using VLBI network. Our goal is (1) to test whether the gigantic flare is still on the empirical relation (2) to detect inpulsive non-thermal emission at the most powerful stellar flare (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band.	GALACTIC POINT SOURCES	4	B	YOHKO TSUBOI		JAP	5	AO5	NON-THERMAL EMISSION AT THE MOST POWERFUL STELLAR FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405011010/	Quick Look
66	1E 1547.0-5408	237.7284	-54.3676	236.761869	-54.21692	248.127922	-33.347549	327.20000551	-0.18012949	271.1663	55415.1611921296	2010-08-07 03:52:07	55415.9633796296	2010-08-07 23:07:16	405024010	51.6728	50	51.6728	51.7928	0	52.1529	2	2	0	1	1	0	0	42.7812	42.7812	69.2999	0	PROCESSED	57552.8870949074	2016-06-13 21:17:25	55793	2011-08-20 00:00:00	55427.247025463	2010-08-19 05:55:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050099	Recently, hard X-ray tails have been detected by INTEGRAL at least up to 150 keV from ~5 magnetars. Suzaku has observed some magnetars during Key Project (AO-4) and ToO observations. As a result, soft X-ray emissions and hard X-ray tails have been detected from ~10 magnetars. This peculiar spectrum is seem to be common in all the magnetars, and we discovered the spectral evolution of magnetars. The remaining problem is to study the spectral difference between the active and quiescent states. Transient magnetar 1E 1547.0-540 was observed with Suzaku in 2009 January, and the extremely hard X-ray tail was detected up to 110 keV with photon index of 1.5, and it is appropriate to study the spectral change. Thus, we propose the observation of 1E 1547.0-5408 with 50 ks.	GALACTIC POINT SOURCES	4	B	HIROYUKI NISHIOKA		JAP	5	AO5	OBSERVATION OF THE HARD X-RAY TAIL AND SOFT X-RAY EMISSION OF AXP 1E 1547.0-5408 IN QUIESCENT STATE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405024010/	Quick Look
67	EMS1150	263.083	-32.7212	262.264926	-32.685689	264.095488	-9.421504	355.27740066	0.39306698	91.2452	55611.9964930556	2011-02-19 23:54:57	55612.6968055556	2011-02-20 16:43:24	405026010	20.9186	20	20.9186	20.9186	0	20.9186	1	1	0	1	1	0	0	17.2639	17.2639	60.5039	0	PROCESSED	57600.9777893518	2016-07-31 23:28:01	55988	2012-03-02 00:00:00	55621.1440740741	2011-03-01 03:27:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050104	Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV.	GALACTIC POINT SOURCES	4	A	YASUYUKI TANAKA		JAP	5	AO5	SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405026010/	Quick Look
68	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
69	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
70	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
71	HER X-1	254.4632	35.2657	254.012163	35.341297	246.023504	57.418254	58.05457552	37.50615868	268.4858	55461.0002083333	2010-09-22 00:00:18	55461.4494675926	2010-09-22 10:47:14	405058030	19.924	20	19.924	19.924	0	20.2438	2	2	0	1	1	0	0	17.5073	17.5073	38.8119	0	PROCESSED	57553.4994560185	2016-06-14 11:59:13	55836	2011-10-02 00:00:00	55470.1508796296	2010-10-01 03:37:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052001	We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity?	GALACTIC POINT SOURCES	4	B	R DIGER STAUBERT		EUR	5	AO5	VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405058030/	Quick Look
72	GX 339-4	255.7015	-48.7852	254.753736	-48.714186	259.571673	-25.859287	338.94105133	-4.32146688	83.6944	55603.7634722222	2011-02-11 18:19:24	55604.2349421296	2011-02-12 05:38:19	405063010	22.4594	100	22.4594	22.4594	0	22.4834	2	2	0	2	1	0	0	19.3287	19.3287	40.7279	0	PROCESSED	57600.9244675926	2016-07-31 22:11:14	55983	2012-02-26 00:00:00	55617.4120601852	2011-02-25 09:53:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052015	We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4	GALACTIC POINT SOURCES	4	A	CLEMENT CABANAC		EUR	5	AO5-TOO	PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063010/	Quick Look
73	GX 339-4	255.7013	-48.7848	254.753541	-48.713785	259.571479	-25.858904	338.94128957	-4.32111913	86.3597	55608.9686111111	2011-02-16 23:14:48	55609.6501967593	2011-02-17 15:36:17	405063020	21.0157	20	21.0157	21.0157	0	21.0157	2	2	0	2	1	0	0	17.5958	17.5958	58.8839	0	PROCESSED	57600.9613773148	2016-07-31 23:04:23	55988	2012-03-02 00:00:00	55621.1561342593	2011-03-01 03:44:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052015	We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4	GALACTIC POINT SOURCES	4	A	CLEMENT CABANAC		EUR	5	AO5-TOO	PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063020/	Quick Look
74	GX 339-4	255.7016	-48.7831	254.753859	-48.712086	259.571491	-25.857192	338.94276391	-4.32024293	90.1024	55616.8233680556	2011-02-24 19:45:39	55617.4487268518	2011-02-25 10:46:10	405063030	19.182	20	19.19	19.198	0	19.182	2	2	0	2	1	0	0	15.684	15.684	54.0259	1	PROCESSED	57601.0471180556	2016-08-01 01:07:51	55996	2012-03-10 00:00:00	55628.1679976852	2011-03-08 04:01:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052015	We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4	GALACTIC POINT SOURCES	4	A	CLEMENT CABANAC		EUR	5	AO5-TOO	PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063030/	Quick Look
75	4U1812-12	273.8053	-12.0935	273.104949	-12.110284	273.784611	11.297146	18.04900466	2.37362039	267.159	55838.1400347222	2011-10-04 03:21:39	55839.9168981482	2011-10-05 22:00:20	406008010	62.0143	60	62.0143	62.0143	0	62.0143	2	2	0	2	1	0	0	53.5441	53.5441	153.5099	1	PROCESSED	57603.3255902778	2016-08-03 07:48:51	56226	2012-10-26 00:00:00	55858.3124768518	2011-10-24 07:29:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060012	Low-Mass X-ray binaries (LMXBs) are known to have soft and hard states, like black hole binaries. Through an analysis of archival Suzaku data of the LMXB Aql X-1 in the hard state, we obtained a clear picture of its accretion geometry; a truncated accretion disk, and a hot corona that Comptonize blackbody photons from the neutron star surface. In order to investigate whether this picture also applies to other LMXBs in the low/hard state, and to better constrain the accretion geometry in comparison with those of black hole binaries, we propose a 60 ksec Suzaku observation of the LMXB 4U 1812-12. This is a valuable object,which is known to reside almost always in the low/hard state.	GALACTIC POINT SOURCES	4	A	SOKI SAKURAI		JAP	6	AO6	REVEALING THE ACCRETION GEOMETRY OF THE LOW/HARD STATE LMXB 4U 1812-12 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406008010/	Quick Look
76	VW HYI	62.3084	-71.2978	62.399199	-71.427045	322.000013	-79.107776	284.88912946	-38.12913625	338.7313	56049.8124305556	2012-05-02 19:29:54	56050.1668171296	2012-05-03 04:00:13	406009040	16.8177	20	16.8257	16.8257	0	16.8177	2	1	0	2	1	0	0	13.9478	13.9478	30.6159	0	PROCESSED	57605.3312847222	2016-08-05 07:57:03	56449	2013-06-06 00:00:00	56083.0857060185	2012-06-05 02:03:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060023	SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate.	GALACTIC POINT SOURCES	4	B	KEI SAITOU		JAP	6	AO6-TOO	TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009040/	Quick Look
77	CYG X-1	299.5916	35.1745	299.121401	35.038023	313.64901	54.223609	71.31236822	3.05181611	279.5001	55839.9245023148	2011-10-05 22:11:17	55840.9169328704	2011-10-06 22:00:23	406013010	3.7027	40	3.832	3.7027	0	40.2718	1	1	0	1	1	0	0	32.9625	32.9625	85.7339	1	PROCESSED	57603.3954166667	2016-08-03 09:29:24	56582	2013-10-17 00:00:00	56212.7247916667	2012-10-12 17:23:42	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060057	We achieved 0.1 s time resolution with enough statistics on accumulating profiles of source brightening and made clear that electron temperature decreases and optical depth increases at the peak of brightness by using the XIS data of Psum mode. Progress to understanding the nature of fast time variability, which has been a mystery for 40 years since its discovery, connected with spectral properties is being made now. However, this property is not confirmed yet in other observations having different time scales of variability and spectral shapes, lacking the XIS data in Psum mode. We propose here another observation of Cyg X-1 with XIS0 1/8 window no burst, XIS1 1/4 window 0.5 s burst,and XIS3 Psum mode for a exposure of 40 ks.	GALACTIC POINT SOURCES	4	A	SHIN'YA YAMADA		JAP	6	AO6	REVEALING THE NATURE OF FAST TIME VARIABILITY OF CYG X-1 WITH SHOT ANALYSIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406013010/	Quick Look
78	AXP 4U 0142+614	26.5682	61.7591	25.700455	61.509234	52.151654	46.394786	129.37061357	-0.42523158	40.384	55811.6552314815	2011-09-07 15:43:32	55812.5731134259	2011-09-08 13:45:17	406031010	38.6497	60	38.6497	38.6497	0	38.6825	2	2	0	2	1	0	0	42.1964	42.1964	79.292	0	PROCESSED	57603.1220138889	2016-08-03 02:55:42	56218	2012-10-18 00:00:00	55851.4406828704	2011-10-17 10:34:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060092	We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI.	GALACTIC POINT SOURCES	4	A	YUJIN NAKAGAWA		JAP	6	AO6-TOO	A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406031010/	Quick Look
79	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
80	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
81	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
82	GX 17+2	274.0108	-14.0482	273.300467	-14.065956	273.933278	9.337698	16.42401351	1.2676957	264.7715	55853.116099537	2011-10-19 02:47:11	55855.5287037037	2011-10-21 12:41:20	406070010	6.5069	100	6.7572	6.5069	0	6.7572	3	2	0	2	1	0	0	87.3599	87.3599	208.4297	3	PROCESSED	57603.5270023148	2016-08-03 12:38:53	56241	2012-11-10 00:00:00	55873.2944444445	2011-11-08 07:04:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062003	The behaviour of dense matter in neutron stars remains enigmatic. To probe this requires accurate measurements of neutron star radii and masses. We have recently shown that broad relativistic Fe emission lines in neutron star low-mass X-ray binaries can be used to constrain the neutron star radius. These sources also provide another tool, kHz quasi-periodic oscillations (QPOs). Combining a measurement of the velocity of the gas in the inner disk (from the Fe line) and the frequency of the kHz QPOs provides a method to measure the neutron star mass if kHz QPOs originate at the inner disk. We propose 100 ksec observations of GX 349+2 and GX 17+2 to provide a detailed Fe line profile. Simultaneously, we will also observe with RXTE to detect the kHz QPOs, allowing us to test this technique.	GALACTIC POINT SOURCES	4	A	EDWARD CACKETT		EUR	6	AO6	EXPLORING THE IRON LINE - KHZ QPO CONNECTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406070010/	Quick Look
83	IGRJ16479-4514	252.0242	-45.1934	251.117904	-45.10536	256.364901	-22.598296	340.16807688	-0.11668459	91.5317	55980.9438194444	2012-02-23 22:39:06	55983.5363541667	2012-02-26 12:52:21	406078010	149.7785	150	149.7865	149.7785	0	149.7865	2	2	0	2	1	0	0	154.7295	154.7295	223.9819	0	PROCESSED	57604.8063888889	2016-08-04 19:21:12	56429	2013-05-17 00:00:00	56062.2788425926	2012-05-15 06:41:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	068014	We propose a 100 ks observation of the Supergiant Fast X-ray Transient (SFXT) with the shortest orbital period, the eclipsing IGRJ16479-4514 (3.3 d), with the main aim of probing its X-ray properties along one entire orbital phase with unprecedented sensitivity. The requested net exposure time indeed translates into an observation almost continuously spanning the whole binary system orbit, allowing for the first time an orbital phase resolved investigation of the X-ray emission properties, which will allow us to study the structure of the supergiant companion (its density and ionization state) and to cast light on the outburst mechanism at work in this new class of transients.	GALACTIC POINT SOURCES	4	A	LARA SIDOLI	ARASH BODAGHEE	EUS	6	AO6	UNVEILING THE MYSTERY OF THE SUPERGIANT FAST X-RAY TRANSIENT WITH THE SHORTEST ORBITAL PERIOD	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406078010/	Quick Look
84	H1743-322	266.5672	-32.235	265.751321	-32.216345	267.052375	-8.828926	357.25482673	-1.83530791	277.9713	56212.4049884259	2012-10-12 09:43:11	56213.3744560185	2012-10-13 08:59:13	407005030	21.361	40	21.3706	21.3722	0	21.361	3	3	0	3	1	0	0	40.615	40.615	83.736	1	PROCESSED	57607.7385416667	2016-08-07 17:43:30	56598	2013-11-02 00:00:00	56232.473275463	2012-11-01 11:21:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070002	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	7	AO7-TOO	MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407005030/	Quick Look
85	CYG X-1	299.5875	35.2031	299.117489	35.06664	313.660052	54.251673	71.33506579	3.06957776	88.7802	56390.0953472222	2013-04-08 02:17:18	56391.9585532407	2013-04-09 23:00:19	407015010	4.1499	85	8.503	4.1499	0	66.4751	2	1	0	1	1	0	0	71.7128	71.7128	160.9658	3	PROCESSED	57611.2046875	2016-08-11 04:54:45	56808	2014-05-31 00:00:00	56402.1391087963	2013-04-20 03:20:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070030	We propose to observe Cyg X-1 for 85 ks, utilizing P-sum mode for XIS3. Our aim is to perform shot analysis, which is originally invented by Negoro et al. 1995 with Ginga, and obtain high-quality wide-band spectra for several phases in less than 1 sec; for example, 0.1 sec before the peak, +/- 0.05 sec at the peak, and after the peak. With these spectra, we will quantify changes in five spectral components: hard Comptonization, soft Comptonization, disk emission, Fe-K lines, and reflection. This will be a clue to know long-standing mystery on rapid variability in black holes.	GALACTIC POINT SOURCES	4	A	SHINYA YAMADA		JAP	7	AO7	INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407015010/	Quick Look
86	Z CAM	126.3	73.123	124.909699	73.28505	106.108743	51.709102	141.36861973	32.62424745	91.2043	56239.0368981482	2012-11-08 00:53:08	56239.7800347222	2012-11-08 18:43:15	407016010	35.852	35	35.852	35.852	0	35.852	2	2	0	2	1	0	0	33.8968	33.8968	64.1939	1	PROCESSED	57607.9797337963	2016-08-07 23:30:49	56631	2013-12-05 00:00:00	56264.602349537	2012-12-03 14:27:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070038	Dwarf novae are a subclass of cataclysmic variables, which sometimes show outbursts. In the outbursts, they are considered to emanate disk winds, but observational evidence had been lacking. Recently, our Suzaku observation of Z Cam during a very transition from quiescence to an outburst revealed clear evidence of the disk wind for the first time, and we were able to study characteristics of the disk wind in detail. Z Cam in quiescence, however, has never been observed with high quality instruments. We, therefore, propose an observation of Z Cam in quiescence in order to study entire behavior of the disk wind throughout different phases, combining the existent Suzaku transition phase data and ASCA archival data taken in other phases.	GALACTIC POINT SOURCES	4	C	KEI SAITOU		JAP	7	AO7	COMPREHENSIVE STUDY FOR THE DISK WIND OF THE DWARF NOVA Z CAM THROUGH OUTBURST CYCLES WITH AN OBSERVATION IN QUIESCENCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407016010/	Quick Look
87	AX J1445.7-5931	221.4519	-59.5275	220.50216	-59.317243	239.705831	-41.083897	316.97780419	0.18867801	281.526	56143.2829513889	2012-08-04 06:47:27	56144.2918865741	2012-08-05 07:00:19	407021010	40.0525	40	41.0682	41.0602	0	40.0525	2	1	0	2	1	0	0	36.8089	36.8089	87.1579	1	PROCESSED	57606.7459722222	2016-08-06 17:54:12	56533	2013-08-29 00:00:00	56167.2116319444	2012-08-28 05:04:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070043	Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution.	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	7	AO7	ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407021010/	Quick Look
88	IGR J17091-3624	257.2866	-36.4073	256.446112	-36.344023	259.498562	-13.427876	349.52701092	2.20940495	283.8915	56202.8636689815	2012-10-02 20:43:41	56203.7202662037	2012-10-03 17:17:11	407037010	42.0759	120	42.0759	42.0837	0	42.0797	3	3	0	3	1	0	0	40.392	40.392	74.0079	0	PROCESSED	57607.2660069444	2016-08-07 06:23:03	56728	2014-03-12 00:00:00	56226.6701388889	2012-10-26 16:05:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070097	We propose a Suzaku observation of "the second GRS 1915+105" IGR J17091-3624 with a high energy resolution and broadband capability. GRS 1915+105 has been considered to be the unique black hole binary that stays at a high mass accretion rate and shows limit-cycle oscillations, but it was recently discovered that the BHC IGR J17091-3624 has exactly the same X-ray variability patterns as GRS 1915+105. This fact suggests an evidence for common physical mechanism in both system. The Suzaku observation will reveal both similarity and difference with GRS 1915+105 from a point of view of broad-band spectral properties and disk wind, and help us understanding of the accretion flow onto a black hole under a high mass accretion rate.	GALACTIC POINT SOURCES	4	B	KAZUTAKA YAMAOKA		JAP	7	AO7	SUZAKU BROADBAND OBSERVATION OF "THE SECOND GRS 1915+105" IGR J17091-3624	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407037010/	Quick Look
89	PG 1658 +440	254.9348	44.0094	254.55381	44.082621	242.595421	66.02047	69.11167171	38.06633743	330.9998	56115.6740972222	2012-07-07 16:10:42	56116.8301041667	2012-07-08 19:55:21	407040010	51.0329	50	51.0329	51.0329	0	51.0329	1	1	0	1	1	0	0	46.6746	46.6746	99.8718	1	PROCESSED	57606.5897222222	2016-08-06 14:09:12	56508	2013-08-04 00:00:00	56142.1447337963	2012-08-03 03:28:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070112	The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects.	GALACTIC POINT SOURCES	4	B	ATSUSHI HARAYAMA		JAP	7	AO7	SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407040010/	Quick Look
90	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
91	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
92	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
93	4U 0352+30	58.8427	31.0494	58.059686	30.903757	63.208913	10.461571	163.07655547	-17.13553633	77.7002	56166.360150463	2012-08-27 08:38:37	56170.0980208333	2012-08-31 02:21:09	407088010	153.4893	150	153.4893	153.4893	0	153.4893	2	2	0	2	1	0	0	140.9919	140.9919	322.9236	3	PROCESSED	57607.0637268518	2016-08-07 01:31:46	56582	2013-10-17 00:00:00	56212.7609722222	2012-10-12 18:15:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072011	After 40 years of studies, surprisingly little is known about accreting pulsars at low-luminosities, yet these may be the most numerous class of neutron star binaries in the Galaxy. Upcoming large-scale surveys will likely reveal many such objects, but to identify them it is crucial to fully understand their properties. X Per, the archetypal source of this class, at 1 kpc from Earth is ideal target for detailed studies. In spite of that X Per is still puzzling. With the proposed program we aim to study X Per in detail, constrain its X-ray spectrum also as a function of the spin phase. Our study will be key to characterize the properties of low-luminosity X-ray pulsars population and will help to identify it in upcoming surveys.	GALACTIC POINT SOURCES	4	B	VICTOR DOROSHENKO		EUR	7	AO7	CRACKING THE X PER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407088010/	Quick Look
94	J1522-5734	230.5286	-57.5816	229.552952	-57.402737	244.521376	-37.577548	322.05619938	-0.4156844	274.4971	56154.6486342593	2012-08-15 15:34:02	56155.0078356482	2012-08-16 00:11:17	407094010	30.0295	25	30.0455	30.0295	0	30.0455	1	1	0	1	1	0	0	23.6862	23.6862	31.0239	0	PROCESSED	57606.8538194444	2016-08-06 20:29:30	56638	2013-12-12 00:00:00	56272.6647222222	2012-12-11 15:57:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072019	The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances.	GALACTIC POINT SOURCES	4	A	MARTINO MARELLI		EUR	7	AO7	SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407094010/	Quick Look
95	4U 0142+61	26.5838	61.7628	25.715895	61.512967	52.16359	46.394147	129.37704782	-0.4200572	82.997	56504.4205902778	2013-07-31 10:05:39	56506.6252430556	2013-08-02 15:00:21	408011010	101.1678	100	101.1678	101.1828	0	101.1828	2	2	0	2	1	0	0	102.4739	102.4739	190.4637	1	PROCESSED	57612.1558680556	2016-08-12 03:44:27	56953	2014-10-23 00:00:00	56587.5059606482	2013-10-22 12:08:35	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080035	A toroidal magnetic field is thought to be formed in neutron star interior after core-collapse supernovae and become an energy source with recently observed X-ray outbursts from magnetars. Since the toroidal field is hidden in the stellar interior, it was thought to be undetectable via the well-known p-pdot method and the cyclotron resonance scattering features. However, a magnetic stress of the magnetar toroidal field is strong enough to distort the stellar shape and produce a free precession in its X-ray pulse timing if the emission pattern deviates from its axis of symmetry. From our analyses of magnetar 4U 0142+61, we found an evidence on the free precession in the hard X-ray component. To confirm and establish this evidence, we propose an additional 100 ks observation of 4U 0142+61.	GALACTIC POINT SOURCES	4	A	TERUAKI ENOTO		JAP	8	AO8	TOROIDAL FIELD INSIDE MAGNETARS OBSERVED WITH SUZAKU TIMING ANALYSES OF ITS FREE PRECESSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408011010/	Quick Look
96	SGR 0501+4516	75.2774	45.2864	74.365802	45.213531	78.849797	22.414701	161.53821228	1.95483036	87.7054	56535.9761574074	2013-08-31 23:25:40	56536.8752662037	2013-09-01 21:00:23	408013010	36.1244	40	36.1244	41.2611	0	41.2452	2	2	0	1	1	0	0	35.7177	35.7177	77.6719	1	PROCESSED	57612.459375	2016-08-12 11:01:30	56974	2014-11-13 00:00:00	56608.6586342593	2013-11-12 15:48:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080040	Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources.	GALACTIC POINT SOURCES	4	B	TERUAKI ENOTO		JAP	8	AO8	ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408013010/	Quick Look
97	SAGITTARIUS A*	266.4146	-29.0065	265.619896	-28.987158	266.840205	-5.604694	359.94434823	-0.0438121	107.0001	56728.6474537037	2014-03-12 15:32:20	56729.1147569445	2014-03-13 02:45:15	408017060	21.1387	20	21.1427	21.1387	0	21.1595	2	2	0	3	1	0	0	20.4844	20.4844	40.368	0	PROCESSED	57614.0078240741	2016-08-14 00:11:16	57113	2015-04-01 00:00:00	56747.6540972222	2014-03-31 15:41:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017060/	Quick Look
98	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
99	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
100	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
101	X 1630-472	248.5012	-47.3939	247.580186	-47.289758	254.085797	-25.132076	336.90807869	0.25236055	88.6321	57077.0625578704	2015-02-24 01:30:05	57078.1140277778	2015-02-25 02:44:12	409007020	5.5296	40	5.547	5.5659	0	5.5296	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6879282407	2016-08-17 16:30:37	57454	2016-03-07 00:00:00	57087.4605208333	2015-03-06 11:03:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090015	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	9	AO9-TOO	MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409007020/	Quick Look
102	H1743-322	266.2607	-32.2285	265.444935	-32.208359	266.789922	-8.828952	357.12541364	-1.6105206	285.4288	56932.6365625	2014-10-02 15:16:39	56933.284837963	2014-10-03 06:50:10	409008010	15.0094	40	15.6012	15.6169	0	15.0094	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6096527778	2016-08-16 14:37:54	57345	2015-11-19 00:00:00	56979.4022569444	2014-11-18 09:39:15	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090015	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	9	AO9-TOO	MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409008010/	Quick Look
103	H1743-322	266.5672	-32.2343	265.751326	-32.215645	267.052358	-8.828226	357.25542532	-1.83494451	273.3773	56939.7339236111	2014-10-09 17:36:51	56940.5245138889	2014-10-10 12:35:18	409008020	19.0006	40	19.0006	19.0145	0	19.0115	3	3	0	3	0	0	0	0	0	0	0	PROCESSED	57616.6317824074	2016-08-16 15:09:46	57345	2015-11-19 00:00:00	56979.407974537	2014-11-18 09:47:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090015	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	9	AO9-TOO	MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409008020/	Quick Look
104	SAGITTARIUS A*	266.4193	-29.0102	265.624572	-28.990881	266.844426	-5.60829	359.94333122	-0.04924818	267.3027	56929.1441550926	2014-09-29 03:27:35	56929.6668402778	2014-09-29 16:00:15	409011010	20.2183	20	20.2183	20.3303	0	20.3543	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5861226852	2016-08-16 14:04:01	56748	2014-04-01 00:00:00	56979.4039814815	2014-11-18 09:41:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090048	With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	9	AO9	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011010/	Quick Look
105	SAGITTARIUS A*	266.4217	-29.0078	265.626986	-28.988492	266.846474	-5.605838	359.94647323	-0.04978962	278.8011	56938.0879861111	2014-10-08 02:06:42	56938.4619097222	2014-10-08 11:05:09	409011020	17.2605	20	17.2605	17.2605	0	17.2605	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6209606482	2016-08-16 14:54:11	56748	2014-04-01 00:00:00	56979.4091087963	2014-11-18 09:49:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090048	With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	9	AO9	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011020/	Quick Look
106	1RXSJ182853.8-241746	277.2212	-24.2932	276.455559	-24.326354	276.570172	-1.017121	8.76671438	-6.19414371	87.3419	57120.5005092593	2015-04-08 12:00:44	57120.8217476852	2015-04-08 19:43:19	409013010	9.7072	12	9.7072	11.8422	0	11.8502	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.9447453704	2016-08-17 22:40:26	57496	2016-04-18 00:00:00	57129.4074189815	2015-04-17 09:46:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090051	We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	B	HIDEYUKI MORI		JAP	9	AO9	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409013010/	Quick Look
107	GK PER	52.8052	43.8974	51.953057	43.727495	61.505862	24.068527	150.96310366	-10.10758836	250.0842	57086.777037037	2015-03-05 18:38:56	57090.7709606482	2015-03-09 18:30:11	409018020	182.886	140	0	0	0	182.886	0	0	0	2	1	0	0	134.9166	134.9166	344.9376	0	PROCESSED	57617.786712963	2016-08-17 18:52:52	57468	2016-03-21 00:00:00	57101.0913657407	2015-03-20 02:11:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090055	A 140-ks observation of the magnetic cataclysmic variable GK Per is proposed. By fitting Suzaku broadband spectra using our multitemperature spectral model of the accretion column, we estimate a white dwarf mass with statistical fitting errors smaller than 5%. The estimated mass will be compared with one obtained from the optical lightcurve fitting method developed and applied by Hachisu and Kato in a series of papers. GK Per is the only known magnetic cataclysmic variable which underwent classical nova explosion (in 1901), and both the mass estimation methods can be applied. Cross-validated WD mass estimation methods will be of importance in studying massive white dwarfs in accretion systems, in relation with the progenitor of type Ia supernovae.	GALACTIC POINT SOURCES	4	A	TAKAYUKI YUASA		JAP	9	AO9	CROSS VALIDATION OF WHITE DWARF MASS ESTIMATION METHODS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409018020/	Quick Look
108	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
109	H 1743+322	266.5667	-32.234	265.750828	-32.215343	267.051923	-8.827937	357.25546218	-1.83442728	271.9807	56924.2942476852	2014-09-24 07:03:43	56927.2779861111	2014-09-27 06:40:18	409059010	119.0885	100	119.0885	119.0965	0	119.5626	3	2	0	1	0	0	0	0	0	0	0	PROCESSED	57616.6267361111	2016-08-16 15:02:30	57310	2015-10-15 00:00:00	56940.6644560185	2014-10-10 15:56:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092020	We propose a triggered Suzaku 100 ks observation of a high-inclination Galactic black hole binary in the hard intermediate state. This will be simultaneous with an already accepted XMM-Newton observation (PI: A. Ingram) to test the Lense-Thirring model for the low frequency quasi-periodic oscillations seen in black hole (and neutron star) binaries. The Suzaku PIN data will enable us to extend the energy range over which the QPO can be studied, allowing us to get much better constraints on the reflection component in the QPO spectrum, and hence to more tightly probe the geometry and emission processes in the regions closest to the black hole.	GALACTIC POINT SOURCES	4	A	MAGNUS AXELSSON		EUR	9	AO9-TOO	TESTING THE LENSE-THIRRING ORIGIN OF THE LOW FREQUENCY QPO IN BLACK HOLE BINARIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409059010/	Quick Look
110	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
111	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
112	PSR J1957+5036	299.4354	50.5474	299.08901	50.41133	327.273287	68.217535	84.58480161	10.99652902	216.5649	55543.4586689815	2010-12-13 11:00:29	55544.0842939815	2010-12-14 02:01:23	405016010	32.469	30	32.485	32.469	0	32.485	2	2	0	2	1	0	0	25.3139	25.3139	54.0339	2	PROCESSED	57554.3965393518	2016-06-15 09:31:01	55959	2012-02-02 00:00:00	55592.9341782407	2011-01-31 22:25:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050047	Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.	GALACTIC POINT SOURCES	4	C	NOBUYUKI KAWAI		JAP	5	AO5	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405016010/	Quick Look
113	CXO J172641.7-354052	261.6769	-35.6761	260.838718	-35.633773	263.074511	-12.434469	352.17176486	-0.26901827	279.4529	56540.003275463	2013-09-05 00:04:43	56540.8015509259	2013-09-05 19:14:14	408021010	37.3165	40	37.3317	37.3349	0	37.3165	2	3	0	2	1	0	0	35.3693	35.3693	68.9659	0	PROCESSED	57612.5112037037	2016-08-12 12:16:08	56956	2014-10-26 00:00:00	56587.7063541667	2013-10-22 16:57:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080100	We propose an additional Suzaku observation of an unclassified gamma-ray source detected with the Fermi LAT telescope. In previous cycles, we found an enigmatic source XSS J12270-4859 to be the first gamma-ray binary among the low-mass X-ray binaries. This proposal aims to find a second source of the same nature for the most prospective target extracted from our catalogue search.	GALACTIC POINT SOURCES	4	C	MASAHIRO TSUJIMOTO		JAP	8	AO8	X-RAY SEARCH OF ANOTHER ENIGMATIC SOURCE IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408021010/	Quick Look
114	CYGNUS X-3	308.2593	40.981	307.808438	40.809488	328.80084	56.880196	79.93230299	0.62160244	252.424	54052.0902893518	2006-11-13 02:10:01	54054.3676388889	2006-11-15 08:49:24	401011010	99.7445	100	99.7462	99.7462	0	99.7445	2	2	0	2	1	0	0	95.3893	95.3893	196.745	1	PROCESSED	57536.1520717593	2016-05-28 03:38:59	54456	2007-12-22 00:00:00	54088.9545023148	2006-12-19 22:54:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010058	We propose an observation of the unusual X-ray binary Cygnus X-3. Cyg X-3 is a final stage of the massive binary stars consisting of a WR(N) star and a compact star. However the nature of the compact star is not well understood. We have fore scientific objective. (A)Determine the Doppler modulation of iron K lines and discuss the binary nature. (2) Determine the iron abundance in the WR wind. (3) Search for the high energy cut off about 100keV of the power law component. (4) Search for the X-ray emission from radio knots. For these four sciences, we propose 100ksec observation of Cyg X-3.	GALACTIC POINT SOURCES	4	C	SHUNJI KITAMOTO		JAP	1	AO1	WIDE BAND OBSERVATION OF CYGNUS X-3 WITH SUZAKU	SPE	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401011010/	Quick Look
115	1RXS J070407.9+26250	106.0341	26.4126	105.260164	26.487679	104.355942	3.767203	190.27497025	14.29877104	282.0717	54548.4868865741	2008-03-23 11:41:07	54549.9862384259	2008-03-24 23:40:11	402008010	58.3157	50	58.3237	58.3157	0	58.3237	1	1	0	1	1	0	0	49.4766	49.4766	129.5278	0	PROCESSED	57541.9808912037	2016-06-02 23:32:29	54933	2009-04-12 00:00:00	54566.326712963	2008-04-10 07:50:28	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020029	Soft Intermediate Polar (IP) is a small group of IPs whose X-ray spectrum is extremely soft compared with general IPs. Recent observations reveal that some soft IPs harbor a soft blackbody component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand possible evolutionary link from IPs to polars, the origin of the soft excess in polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure their temperature and flux systematically.	GALACTIC POINT SOURCES	4	C	MANABU ISHIDA		JAP	2	AO2	OBSERVATIONS OF SOFT INTERMEDIATE POLARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402008010/	Quick Look
116	U SCO	245.6288	-17.8156	244.907071	-17.699112	246.808077	3.684973	357.72079613	21.90901194	93.2747	55233.0102430556	2010-02-06 00:14:45	55234.2918865741	2010-02-07 07:00:19	404018010	46.0764	20	46.0764	46.0764	0	46.0764	2	2	0	2	1	0	0	37.6117	37.6117	110.7199	1	PROCESSED	57550.518599537	2016-06-11 12:26:47	55617	2011-02-25 00:00:00	55250.1559375	2010-02-23 03:44:33	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040057	We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each.	GALACTIC POINT SOURCES	4	A	DAI TAKEI		JAP	4	AO4-TOO	TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404018010/	Quick Look
117	II PEG	358.7744	28.6284	358.137778	28.350132	11.171995	26.557383	108.23861581	-32.63076231	231.1411	56301.1877314815	2013-01-09 04:30:20	56303.6487962963	2013-01-11 15:34:16	407038010	17.0176	100	111.5065	111.5145	0	17.0176	3	3	0	3	1	0	0	107.9058	107.9058	212.6198	2	PROCESSED	57608.5074305556	2016-08-08 12:10:42	56724	2014-03-08 00:00:00	56363.602037037	2013-03-12 14:26:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070102	We propose a Suzaku observation of the powerful flare star II Peg with the high sensitivity of HXD. MAXI/GSC results from 2009 to 2011 show that this source exhibits the highest flaring activity with the largest luminosities and the largest fluxes. Then detection of the non-thermal emission is the most expected from this source at the on-set of a flare. We are to observe this target simultaneously with radio, infrared, optical, and X-ray bands for the first time. Our goal is (1) to detect impulsive non-thermal emission at the powerful II Peg flare (2) to obtain wide-band SED variability from radio to hard X-ray band, and (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band.	GALACTIC POINT SOURCES	4	C	YOHKO TSUBOI		JAP	7	AO7	NON-THERMAL EMISSION ON THE POWERFUL STELLAR FLARE FROM II PEG	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407038010/	Quick Look
118	4U 1820-30	275.9218	-30.4206	275.118218	-30.447383	275.13391	-7.085348	2.73584989	-7.94270191	269.3964	55116.6321064815	2009-10-12 15:10:14	55117.1759143518	2009-10-13 04:13:19	404069060	24.6687	100	0	24.6687	0	24.6687	0	1	0	2	1	0	0	16.9505	16.9505	46.978	0	PROCESSED	57548.8754861111	2016-06-09 21:00:42	55507	2010-11-07 00:00:00	55131.3693518518	2009-10-27 08:51:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069060/	Quick Look
119	CYGNUS X-1	299.5895	35.2721	299.119922	35.135631	313.702443	54.316106	71.39489928	3.10413213	91.3103	54929.2562847222	2009-04-08 06:09:03	54929.8224421296	2009-04-08 19:44:19	404075020	21.3361	300	21.3361	21.3361	0	21.3361	2	1	0	2	1	0	0	13.1258	13.1258	48.914	0	PROCESSED	57546.0782638889	2016-06-07 01:52:42	54922	2009-04-01 00:00:00	54949.4903125	2009-04-28 11:46:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075020/	Quick Look
120	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
121	1RXSJ173905.2-392615	264.7748	-39.4365	263.906258	-39.409033	265.79264	-16.071333	350.35081336	-4.37467046	271.2006	56188.8237384259	2012-09-18 19:46:11	56189.3446990741	2012-09-19 08:16:22	407029010	22.0638	15	22.0718	22.0638	0	22.0718	1	1	0	1	1	0	0	18.2515	18.2515	44.9999	0	PROCESSED	57607.0891898148	2016-08-07 02:08:26	56584	2013-10-19 00:00:00	56218.4994212963	2012-10-18 11:59:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070052	We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	C	HIDEYUKI MORI		JAP	7	AO7	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407029010/	Quick Look
122	U GEM IN QUIECSECNCE	118.777	21.9977	118.037172	22.130129	116.517698	1.166962	199.22882002	23.39765052	280.879	56041.5636921296	2012-04-24 13:31:43	56044.5765856482	2012-04-27 13:50:17	407034010	119.1136	120	119.1136	119.1136	0	119.1136	3	2	0	2	1	0	0	102.8354	102.8354	260.306	1	PROCESSED	57605.3496064815	2016-08-05 08:23:26	56434	2013-05-22 00:00:00	56068.6228356482	2012-05-21 14:56:53	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070065	It has been believed that the optically thin boundary layer in dwarf novae (DNe) turns into optically thick state in outburst, and, as a result, hard optically thin X-ray emission becomes weaker than in quiescence. This theory was verified in multi-waveband observations of SS Cyg. The DN U Gem, however, does not follow this scenario, and the hard X-ray intensity increases in outburst as well as soft X-ray emission. We propose ToO observations of U Gem both in quiescence and in outburst in order to understand behavior of DNe in X-rays in general, by means of detailed spectroscopy of the soft disk blackbody component, the hard component reflected off the white dwarf, and a 6.4 keV iron line. This study eventually enables us to understand the origin of the Galactic Ridge X-ray Emission.	GALACTIC POINT SOURCES	4	B	TAKAYUKI HAYASHI		JAP	7	AO7-TOO	OBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407034010/	Quick Look
123	1RXS J180340.0+40121	270.932	40.2098	270.526529	40.206239	271.586717	63.644696	66.8583442	25.77561005	157.538	54478.0290972222	2008-01-13 00:41:54	54479.1877777778	2008-01-14 04:30:24	402009010	53.0907	50	53.0907	53.0907	0	53.0907	1	1	0	1	1	0	0	44.3489	44.3489	100.0959	3	PROCESSED	57541.2965625	2016-06-02 07:07:03	54864	2009-02-02 00:00:00	54490.0707291667	2008-01-25 01:41:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020029	Soft Intermediate Polar (IP) is a small group of IPs whose X-ray spectrum is extremely soft compared with general IPs. Recent observations reveal that some soft IPs harbor a soft blackbody component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand possible evolutionary link from IPs to polars, the origin of the soft excess in polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure their temperature and flux systematically.	GALACTIC POINT SOURCES	4	C	MANABU ISHIDA		JAP	2	AO2	OBSERVATIONS OF SOFT INTERMEDIATE POLARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402009010/	Quick Look
124	SAGITTARIUS A*	266.4179	-29.0156	265.623138	-28.996274	266.843332	-5.613719	359.938084	-0.05101613	284.9967	56561.9008101852	2013-09-26 21:37:10	56562.4828587963	2013-09-27 11:35:19	408017040	18.3285	20	18.3422	18.3285	0	18.3422	3	2	0	3	1	0	0	18.9519	18.9519	50.282	0	PROCESSED	57612.7244560185	2016-08-12 17:23:13	56956	2014-10-26 00:00:00	56588.4972222222	2013-10-23 11:56:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017040/	Quick Look
125	SAGITTARIUS A*	266.4147	-29.0052	265.620004	-28.985859	266.84026	-5.603392	359.94550345	-0.04320951	106.9995	56723.0565277778	2014-03-07 01:21:24	56723.5487384259	2014-03-07 13:10:11	408017050	21.9949	20	21.9949	22.0029	0	22.0144	1	1	0	1	1	0	0	15.862	15.862	42.5199	1	PROCESSED	57613.9706828704	2016-08-13 23:17:47	57100	2015-03-19 00:00:00	56734.6444328704	2014-03-18 15:27:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017050/	Quick Look
126	V2301 OPH	270.1519	8.1612	269.551065	8.161911	270.165981	31.601449	34.53664844	14.98247082	262.0703	56573.9878356482	2013-10-08 23:42:29	56576.0002893518	2013-10-11 00:00:25	408024010	40.1356	150	40.1356	40.1356	0	40.1356	2	2	0	2	1	0	0	65.6843	65.6843	173.8587	1	PROCESSED	57612.9068981482	2016-08-12 21:45:56	57184	2015-06-11 00:00:00	56596.5744907407	2013-10-31 13:47:16	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080107	It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion.	GALACTIC POINT SOURCES	4	A	TAKAYUKI HAYASHI		JAP	8	AO8	MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408024010/	Quick Look
127	SGR 1900+14	286.7986	9.3873	286.201777	9.308221	289.568815	31.69386	43.07377535	0.80526184	82.6704	54947.7664814815	2009-04-26 18:23:44	54949.0807175926	2009-04-28 01:56:14	404077010	53.1374	50	53.3934	53.3934	0	53.1374	2	2	0	2	1	0	0	42.1011	42.1011	113.5479	1	PROCESSED	57546.4694444444	2016-06-07 11:16:00	54922	2009-04-01 00:00:00	54973.4547222222	2009-05-22 10:54:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	4	AO4	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404077010/	Quick Look
128	1E1207.4-5209	182.5062	-52.436	181.851861	-52.157726	209.149793	-45.774623	296.5458403	9.92149786	302.4939	53946.5682060185	2006-07-30 13:38:13	53948.2603587963	2006-08-01 06:14:55	401030010	96.3519	120	96.3519	102.2784	96.3679	96.3519	3	2	3	3	1	0	0	94.0498	94.0498	135.3799	1	PROCESSED	57535.1230787037	2016-05-27 02:57:14	54750	2008-10-11 00:00:00	54132.8187268518	2007-02-01 19:38:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010152	1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object.	GALACTIC POINT SOURCES	4	B	ATSUMASA YOSHIDA		JAP	1	AO1	A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401030010/	Quick Look
129	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
130	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
131	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
132	SAGITTARIUS A*	266.4197	-29.0062	265.624997	-28.986883	266.844677	-5.604282	359.94692786	-0.04746309	282.0043	56539.5310416667	2013-09-04 12:44:42	56540.000162037	2013-09-05 00:00:14	408017010	19.4579	20	19.4789	19.4579	0	19.4709	2	2	0	2	1	0	0	20.6423	20.6423	40.5219	0	PROCESSED	57612.4854976852	2016-08-12 11:39:07	56974	2014-11-13 00:00:00	56608.6493981482	2013-11-12 15:35:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017010/	Quick Look
133	J1620-4927	245.1748	-49.4572	244.240353	-49.338216	252.062857	-27.548671	333.89109656	0.40900491	274.3002	56157.8029513889	2012-08-18 19:16:15	56158.5203356482	2012-08-19 12:29:17	407091010	29.2601	25	29.2601	29.2841	0	29.2601	1	1	0	1	1	0	0	29.8402	29.8402	61.9679	0	PROCESSED	57606.8716898148	2016-08-06 20:55:14	56592	2013-10-27 00:00:00	56226.6098148148	2012-10-26 14:38:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072019	The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances.	GALACTIC POINT SOURCES	4	A	MARTINO MARELLI		EUR	7	AO7	SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407091010/	Quick Look
134	1FGL J2339.7-0531	354.9077	-5.5469	354.264388	-5.824081	353.120926	-3.069352	81.34836456	-62.4702773	67.4026	55741.5915625	2011-06-29 14:11:51	55743.8092361111	2011-07-01 19:25:18	406007010	104.0914	100	104.0914	104.0914	0	104.0994	2	2	0	2	1	0	0	92.9022	92.9022	191.5837	2	PROCESSED	57602.4861805556	2016-08-02 11:40:06	56144	2012-08-05 00:00:00	55775.4025925926	2011-08-02 09:39:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060007	We propose to observe an unidentified Fermi source (1FGL J2339.7-0531) in the first-year Fermi catalog to search for the first ``radio-quiet'' Gamma-ray emitting millisecond pulsar. The Fermi source has a candidate X-ray counterpart from Chandra data and its X-ray and Gamma-ray properties are consistent with known Gamma-ray pulsars. This system is likely in a low-mass X-ray binary system based on optical observations. Both X-ray and optical observations show clear variability. We propose to observe the Chandra source with Suzaku to search for the possible orbital period and to study its X-ray spectrum in detail. The results will provide a better insight into the high-energy emission processes in the magnetosphere of millisecond pulsars.	GALACTIC POINT SOURCES	4	A	ALBERT KONG	JUN KATAOKA	JAP	6	AO6	REVEALING THE NATURE OF AN UNIDENTIFIED FERMI SOURCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406007010/	Quick Look
135	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
136	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
137	1FGL J1715.2-3319	258.713	-33.4282	257.892464	-33.371742	260.432113	-10.360749	352.62684601	3.01774525	99.0737	56002.5629166667	2012-03-16 13:30:36	56003.3750810185	2012-03-17 09:00:07	406024010	32.165	30	32.165	32.165	0	32.165	2	2	0	2	1	0	0	27.9848	27.9848	70.166	0	PROCESSED	57604.9296064815	2016-08-04 22:18:38	56386	2013-04-04 00:00:00	56019.2516435185	2012-04-02 06:02:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060087	We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object.	GALACTIC POINT SOURCES	4	C	MASANORI OHNO		JAP	6	AO6	SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406024010/	Quick Look
138	1RXSJ135341.1-664002	208.4233	-66.67	207.481758	-66.423993	237.082372	-50.124321	309.05087215	-4.54070575	288.5314	55774.1593055556	2011-08-01 03:49:24	55774.6939236111	2011-08-01 16:39:15	406036010	23.2679	20	23.2759	23.2679	0	23.2759	1	1	0	1	1	0	0	22.4241	22.4241	46.1839	0	PROCESSED	57602.7124189815	2016-08-02 17:05:53	56166	2012-08-27 00:00:00	55802.4628472222	2011-08-29 11:06:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060097	We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray.	GALACTIC POINT SOURCES	4	B	HIROMITSU TAKAHASHI		JAP	6	AO6	SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406036010/	Quick Look
139	GT MUS	174.8799	-65.348	174.296149	-65.070756	218.231345	-58.061728	295.52044001	-3.51633969	94.8564	54446.4736689815	2007-12-12 11:22:05	54449.187662037	2007-12-15 04:30:14	402095010	93.3087	80	93.3087	93.3087	0	93.3087	2	2	0	2	1	0	0	94.6965	94.6965	234.4699	3	PROCESSED	57540.9318287037	2016-06-01 22:21:50	54828	2008-12-28 00:00:00	54460.7707060185	2007-12-26 18:29:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022020	We propose to perform broad-band X-ray spectroscopy of the RS CVn-like system GT Muscae, with the aim to study the thermal and non-thermal components of its X-ray emitting plasma. Our target is a known hard X-ray source, detected with Uhuru and recently with Integral/IBIS in the 20-40 keV band, but lacking a dedicated observation with modern X-ray spectrometers. The proposed observation will allow us to investigate both the quiescent and flaring states of this complex (possibly interacting) binary system, by means of a variability study and a time-resolved spectral analysis of its X-ray emission. We aim to detect and constrain the non-thermal hard X-ray emission component, and to search for a possible Fe Kalpha line emission, thanks to the superb broad-band spectral capabilities of Suzaku.	GALACTIC POINT SOURCES	4	B	ANTONIO MAGGIO		EUR	2	AO2	BROAD-BAND X-RAY SPECTROSCOPY OF AN EXTREMELY ACTIVE CORONAL SOURCE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402095010/	Quick Look
140	LMC X-2	80.025	-71.9941	80.229686	-72.041872	298.35324	-83.539153	283.14092563	-32.7117801	313.3022	53849.381712963	2006-04-24 09:09:40	53850.7731365741	2006-04-25 18:33:19	401012010	56.152	60	56.1657	56.1657	56.152	56.16	2	2	2	2	1	0	0	73.408	73.408	120.1938	1	PROCESSED	57533.5735300926	2016-05-25 13:45:53	54394	2007-10-21 00:00:00	53907.6288078704	2006-06-21 15:05:29	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010090	We propose the Suzaku observation of LMC X-2, to detect the slim disk structure in its flaring branch. The luminosity of LMC X-2 is always as luminous as the Eddington limit, and the absorption is so low that the energy spectrum can be observed over the 0.2-30 keV energy range. Then, LMC X-2 is the best target to study whether the disk structure becomes the slim disk or not.	GALACTIC POINT SOURCES	4	B	HIROMITSU TAKAHASHI		JAP	1	AO1	DETECTION OF SLIM-DISK STRUCTURE FROM LOW-MASS X-RAY BINARY LMC X-2	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401012010/	Quick Look
141	AM HERCULES	274.126	49.8084	273.81383	49.78911	279.176537	73.11739	77.81082077	25.81903319	234.8814	54768.8590162037	2008-10-29 20:36:59	54771.3043287037	2008-11-01 07:18:14	403007010	108.4965	100	108.5045	108.5045	0	108.4965	2	2	0	2	1	0	0	94.4671	94.4671	211.2577	3	PROCESSED	57544.3392476852	2016-06-05 08:08:31	55156	2009-11-21 00:00:00	54788.4722222222	2008-11-18 11:20:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030021	We propose the observation of the proto-type magnetic catacrysmic variables, AM Hercules, to search for possible hard X-ray tail on the thermal emission with Suzaku. To reduce the systematics of the estimation of the GSO background in the analyses, we propose the additional observation of blank sky near the object.	GALACTIC POINT SOURCES	4	C	YUKIKATSU TERADA		JAP	3	AO3	NON THERMAL EMISSION FROM THE POLAR AM HERCULES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403007010/	Quick Look
142	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
143	EP DRA	286.7359	69.1573	286.793684	69.076999	30.014466	83.210835	100.08892772	23.87463538	44.5637	57164.4409953704	2015-05-22 10:35:02	57166.2856365741	2015-05-24 06:51:19	410006010	80.2346	80	80.2346	80.2426	0	80.2426	2	2	0	2	1	0	0	67.9585	67.9585	155.5819	1	PROCESSED	57618.7517939815	2016-08-18 18:02:35	57558	2016-06-19 00:00:00	57176.3159027778	2015-06-03 07:34:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	100018	It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar mass (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar mass and approach 3.3 solar mass. We will get observational relations between WD mass and radius for proposed targets with Suzaku. With WD masses dynamically measured, we can estimate the WD radii without any theoretical mass-radius relation. We will be able to, for the first time, observationally investigate the influence of magnetic field on EOS in WDs and the WD mass-radius relation by the estimating WD radii and masses.	GALACTIC POINT SOURCES	4	A	TAKAYUKI HAYASHI		JAP	10	AO10	CONSTRAINT ON MASS-RADIUS RELATION OF HIGHLY MAGNETIZED WHITE DWARFS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410006010/	Quick Look
144	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
145	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
146	VW HYI	62.2833	-71.2901	62.373607	-71.419454	322.048735	-79.101508	284.88594452	-38.13999051	181.9815	55894.1004513889	2011-11-29 02:24:39	55895.1821759259	2011-11-30 04:22:20	406009010	70.0834	60	70.0914	70.0834	0	70.0914	2	2	0	2	1	0	0	64.9701	64.9701	93.4468	1	PROCESSED	57604.0242939815	2016-08-04 00:34:59	56274	2012-12-13 00:00:00	55907.1562615741	2011-12-12 03:45:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060023	SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate.	GALACTIC POINT SOURCES	4	B	KEI SAITOU		JAP	6	AO6-TOO	TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009010/	Quick Look
147	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
148	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
149	G11.2-0.3	272.8676	19.433	272.324919	19.420376	273.677117	42.836704	46.34586116	17.29738119	77.6432	53834.4626041667	2006-04-09 11:06:09	53835.6634143518	2006-04-10 15:55:19	401010010	43.9846	50	43.9926	43.9846	43.9926	43.9926	2	2	2	2	1	0	0	37.3879	37.3879	83.6799	1	PROCESSED	57533.4279166667	2016-05-25 10:16:12	54397	2007-10-24 00:00:00	53905.4671875	2006-06-19 11:12:45	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010049	The PSR 1811-1925 in a historical supernova remnant G11.2-0.3 has its characteristic age as 10 times longer than the age of the remnant. The pulsar has its period 64 ms and the hard spectrum. We suggest that the pulsar shows the signs of having the small magnetic field. The SUZAKU observation must give the answer for this hypothesis. First, HXD allows us to observe the spectrum in the high energy range, and if the cut-off would be observed, the magnetic fields of pulsar will be estimate. Seconds, XIS has the great energy resolution to determine the abundance of the shell. This would let us estimate the mass of the progenitor. Third, HXD provides the new spin down rate observation. Then, we can make sure the constancy of the spin down rate. The pulsar age mystery must be solved by SUZAKU.	GALACTIC POINT SOURCES	4	C	ASAMI HAYATO		JAP	1	AO1	CLEARING UP THE MECHANISM OF THE PSR J1811-1925 IN SNR G11.2-0.3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401010010/	Quick Look
150	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
151	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
152	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
153	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
154	HESS J1731-347	263.0179	-34.7706	262.185573	-34.73474	264.142481	-11.47104	353.53173388	-0.68198005	79.8005	54154.7807060185	2007-02-23 18:44:13	54155.7432291667	2007-02-24 17:50:15	401099010	40.6189	38	40.6269	40.6189	0	40.6269	2	2	0	2	1	0	0	34.6479	34.6479	83.1559	0	PROCESSED	57537.4739351852	2016-05-29 11:22:28	54528	2008-03-03 00:00:00	54160.3931944444	2007-03-01 09:26:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012042	The hard (Gamma=2.0) TeV source HESS J1731-347 discovered in the H.E.S.S. Galactic plane survey has an intriguing possible counterpart seen in ROSAT survey data. The X-ray data show an unidentified, extended nebular structure with a hard spectrum, in close coincidence to the TeV source. It is plausible to assume that the same energetic particle population is responsible for the emission in both bands. Suzaku is optimally suited to establish the likely non-thermal nature of the X-ray spectrum and to search for the high-energy end of the emitting particle spectrum, which is likely visible in the HXD domain. The observations will help to clarify the nature of HESS J1731-347, which may be a new type of Galactic particle accelerator.	GALACTIC POINT SOURCES	4	A	GERD PUEHLHOFER		EUR	1	AO1	THE HIGH ENERGY PARTICLE SPECTRUM OF THE TEV/X-RAY NEBULA HESS J1731-347	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401099010/	Quick Look
155	PSR B1259-63	195.6732	-63.8823	194.883764	-63.613652	227.720536	-50.935927	304.17036556	-1.03761834	285.8945	54294.6568865741	2007-07-13 15:45:55	54295.3459953704	2007-07-14 08:18:14	402014040	22.9149	20	22.9149	22.9149	0	22.9149	2	2	0	2	1	0	0	21.0706	21.0706	59.4959	1	PROCESSED	57539.2651273148	2016-05-31 06:21:47	54709	2008-08-31 00:00:00	54339.4142592593	2007-08-27 09:56:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014040/	Quick Look
156	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
157	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
158	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
159	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
160	SU AUR	73.9934	30.5715	73.195309	30.492884	76.133121	7.898373	172.51103259	-7.93275707	85.9197	54339.1713541667	2007-08-27 04:06:45	54340.7502199074	2007-08-28 18:00:19	402090010	57.3034	55	57.3114	57.3034	0	57.3114	2	2	0	2	1	0	0	54.3848	54.3848	136.4018	1	PROCESSED	57539.9114699074	2016-05-31 21:52:31	54723	2008-09-14 00:00:00	54350.6381597222	2007-09-07 15:18:57	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022007	We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra.	GALACTIC POINT SOURCES	4	A	JURGEN SCHMITT		EUR	2	AO2	ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402090010/	Quick Look
161	MARS-P1	102.8773	25.1625	102.108873	25.222717	101.648232	2.240772	190.24974394	11.19384085	298.0037	54559.3414814815	2008-04-03 08:11:44	54559.4099421296	2008-04-03 09:50:19	403006010	2.9048	100	2.9048	2.9128	0	2.9128	1	1	0	1	1	0	0	2.9096	2.9096	5.9119	0	PROCESSED	57542.0343981482	2016-06-03 00:49:32	54953	2009-05-02 00:00:00	54577.0446875	2008-04-21 01:04:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006010/	Quick Look
162	MARS-P4	103.0016	25.1536	102.233284	25.214407	101.761173	2.241936	190.30618657	11.29219101	298.0476	54559.5767592593	2008-04-03 13:50:32	54559.6599421296	2008-04-03 15:50:19	403006040	2.2882	100	2.2882	2.2882	0	2.2882	1	1	0	1	1	0	0	2.01	2.01	7.1839	0	PROCESSED	57542.0411226852	2016-06-03 00:59:13	54953	2009-05-02 00:00:00	54577.0528935185	2008-04-21 01:16:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006040/	Quick Look
163	MARS-P15	103.4611	25.1019	102.69331	25.164885	102.180485	2.228357	190.53184536	11.64832678	298.2083	54560.4934375	2008-04-04 11:50:33	54560.5766666667	2008-04-04 13:50:24	403006150	3.831	100	3.839	3.831	0	3.847	1	1	0	1	1	0	0	3.1928	3.1928	7.1839	1	PROCESSED	57542.0622222222	2016-06-03 01:29:36	54953	2009-05-02 00:00:00	54580.5809837963	2008-04-24 13:56:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006150/	Quick Look
164	AM HERCULES BGD	282.0964	47.9785	281.757583	47.920958	294.678535	70.385314	77.40285415	20.2844947	234.9986	54771.3072106482	2008-11-01 07:22:23	54772.3438310185	2008-11-02 08:15:07	403008010	44.3601	40	44.3681	44.3601	0	44.3921	2	2	0	2	1	0	0	40.4115	40.4115	89.5519	1	PROCESSED	57544.3170833333	2016-06-05 07:36:36	55154	2009-11-19 00:00:00	54788.4288541667	2008-11-18 10:17:33	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030021	We propose the observation of the proto-type magnetic catacrysmic variables, AM Hercules, to search for possible hard X-ray tail on the thermal emission with Suzaku. To reduce the systematics of the estimation of the GSO background in the analyses, we propose the additional observation of blank sky near the object.	GALACTIC POINT SOURCES	4	C	YUKIKATSU TERADA		JAP	3	AO3	NON THERMAL EMISSION FROM THE POLAR AM HERCULES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403008010/	Quick Look
165	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
166	XTE J1759-220	269.9393	-22.0118	269.18599	-22.009675	269.934127	1.429042	7.5831003	0.77858469	86.479	54566.5188773148	2008-04-10 12:27:11	54567.6460532407	2008-04-11 15:30:19	403072010	48.961	50	49.361	49.425	0	48.961	2	2	0	2	1	0	0	43.9129	43.9129	97.3639	1	PROCESSED	57542.2983912037	2016-06-03 07:09:41	54953	2009-05-02 00:00:00	54580.4766550926	2008-04-24 11:26:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032012	Dipping low-mass X-ray binaries (LMXBs), a subclass of LMXBs that are viewed close to the disk plane, provide us with a rare opportunity to probe the structure of accretion disks. This was nicely illustrated with the discovery of Fe XXV and Fe XXVI absorption lines in all the dipping LMXBs observed with XMM and Chandra. It revealed the existence of a highly-ionized atmosphere above the disk which is likely present in any LMXB but only detectable in the ones seen close to edge-on. We propose to observe two recently discovered dipping binaries with Suzaku, to constrain the basic astrophysical properties (orbital period, distance, variability, high energy cutoff, etc) of these yet poorly observed sources, and to further investigate the ionized atmosphere in X-ray binaries in general.	GALACTIC POINT SOURCES	4	B	LAURENCE BOIRIN		EUR	3	AO3	NEW DIPPING X-RAY BINARIES TO PROBE ACCRETION DISKS AND THEIR IONIZED ATMOSPHER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403072010/	Quick Look
167	RXJ0007.0+7302	1.8916	72.9843	1.226338	72.706084	53.083805	60.867639	119.68700382	10.38954096	241.7328	55204.6112847222	2010-01-08 14:40:15	55207.0675231482	2010-01-11 01:37:14	404011010	105.3739	100	105.3739	105.3739	0	106.9714	2	2	0	1	1	0	0	58.5644	58.5644	212.2059	2	PROCESSED	57550.1958564815	2016-06-11 04:42:02	55587	2011-01-26 00:00:00	55768.9633333333	2011-07-26 23:07:12	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040054	We propose to observe the gamma-ray pulsar and itswind nebula (PWN) in the supernova remnant CTA1 with SUZAKU. Observations in X-ray wavebands are crucial to study non-thermal processes of PWNe. Its flux and spectral shape provide us important information about the energy distribution of the accelerated particles and the strength of the magnetic field. Observations made by Suzaku-HXD will constrain the X-ray spectrum above 20keV from the PWN for the first time. The high spectral resolution of XIS will allow us to search for metal lines, which tell us circumstance of the emission region. In addition, we will probably able to detect X-ray pulsation, which has notbeen detected yet, using XIS timing mode.	GALACTIC POINT SOURCES	4	C	JUMPEI TAKATA		JAP	4	AO4	X-RAY OBSERVATIONS OF GAMMA-RAY PULSAR AND ITS WIND NEBULA IN CTA1	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404011010/	Quick Look
168	FO AQR	334.4646	-8.2931	333.805898	-8.543636	333.309968	2.14088	53.06192299	-49.11309098	76.4186	54987.3437152778	2009-06-05 08:14:57	54988.5536921296	2009-06-06 13:17:19	404032010	46.0846	40	46.0846	46.0846	0	46.0846	2	2	0	2	1	0	0	33.4993	33.4993	104.5299	0	PROCESSED	57547.5153356482	2016-06-08 12:22:05	55366	2010-06-19 00:00:00	54998.3271064815	2009-06-16 07:51:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040113	We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.	GALACTIC POINT SOURCES	4	A	TAKAYUKI YUASA		JAP	4	AO4	SURVEY OBSERVATION OF INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404032010/	Quick Look
169	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
170	4U 1820-30	275.9248	-30.4209	275.121217	-30.447698	275.136502	-7.085754	2.73676025	-7.94514519	265.9319	55088.3645833333	2009-09-14 08:45:00	55088.8141087963	2009-09-14 19:32:19	404069020	21.0373	20	21.0373	21.0373	0	21.0373	1	1	0	1	1	0	0	17.17	17.17	38.8319	0	PROCESSED	57548.569837963	2016-06-09 13:40:34	55469	2010-09-30 00:00:00	55103.4457407407	2009-09-29 10:41:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069020/	Quick Look
171	CYGNUS X-1	299.6277	35.1371	299.157204	35.000471	313.675062	54.178467	71.29581116	3.00713364	246.5433	55145.8193981482	2009-11-10 19:39:56	55146.4377199074	2009-11-11 10:30:19	404075160	26.0222	300	26.0222	26.0382	0	26.0265	2	1	0	2	1	0	0	18.2505	18.2505	53.416	0	PROCESSED	57549.2577199074	2016-06-10 06:11:07	54922	2009-04-01 00:00:00	55176.2027430556	2009-12-11 04:51:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075160/	Quick Look
172	IGR J15094-6649	227.3484	-66.8278	226.235673	-66.63712	247.091848	-46.74399	315.91945149	-7.50109233	90.4626	55588.7031365741	2011-01-27 16:52:31	55589.5557638889	2011-01-28 13:20:18	405007010	49.4612	50	49.4832	49.4752	0	49.4612	2	2	0	2	1	0	0	48.0185	48.0185	73.6599	0	PROCESSED	57600.7830092593	2016-07-31 18:47:32	55990	2012-03-04 00:00:00	55621.2282291667	2011-03-01 05:28:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050025	The all-sky survey in hard X-rays with INTEGRAL has been finding new magnetic Cataclysmic Variables. Among them, we propose Suzaku observations of five Intermediate Polars (IPs) which have no detailed follow-up spectroscopy in the hard X-ray band up to now. The wide-band energy coverage of Suzaku, therefore, is definitely useful to extract physical information from their spectra since, generally, the vFv spectrum of an IP peaks at E=20-50 keV and strong intrinsic absorption (nH=1E22-23 cm-2). By fitting the spectrum with our numerical model, we estimate a plasma temperature and an Fe abundance, and furthermore, a white dwarf mass which is one of the most basic and important parameter of a binary system.	GALACTIC POINT SOURCES	4	C	TAKAYUKI YUASA		JAP	5	AO5	ESTIMATE MASSES OF NEWLY-FOUND MAGNETIC WHITE DWARFS BASED ON HARD X-RAY CONTINUUM AND FE EMISSION LINES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405007010/	Quick Look
173	XSS J16537-1905	253.8855	-18.1447	253.157456	-18.065723	254.650655	4.44189	2.56699105	15.52634316	96.7569	55602.7046412037	2011-02-10 16:54:41	55603.1488657407	2011-02-11 03:34:22	405032010	20.0243	20	20.0323	20.0403	0	20.0243	2	2	0	2	1	0	0	18.1528	18.1528	38.3439	0	PROCESSED	57600.887337963	2016-07-31 21:17:46	55983	2012-02-26 00:00:00	55617.4104282407	2011-02-25 09:51:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050116	Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	5	AO5	QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405032010/	Quick Look
174	10 LAC	339.8111	39.0619	339.249017	38.801118	0.373962	43.220063	96.65409432	-16.97165842	81.7456	55344.5001967593	2010-05-28 12:00:17	55345.0690162037	2010-05-29 01:39:23	405060010	25.0284	25	25.0284	25.0284	0	25.0284	2	2	0	2	1	0	0	21.7431	21.7431	49.1359	2	PROCESSED	57551.6393287037	2016-06-12 15:20:38	55731	2011-06-19 00:00:00	55365.1824305556	2010-06-18 04:22:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052005	We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models.	GALACTIC POINT SOURCES	4	A	LIDIA OSKINOVA		EUR	5	AO5	STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405060010/	Quick Look
175	VW HYI	62.3086	-71.2914	62.399129	-71.420645	322.033067	-79.109175	284.88209314	-38.1323503	276.4367	55986.5687962963	2012-02-29 13:39:04	55987.2501273148	2012-03-01 06:00:11	406009030	20.1097	20	20.1097	20.1097	0	20.1097	2	2	0	2	1	0	0	20.5712	20.5712	58.8579	1	PROCESSED	57604.7590972222	2016-08-04 18:13:06	56385	2013-04-03 00:00:00	56018.9417824074	2012-04-01 22:36:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060023	SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate.	GALACTIC POINT SOURCES	4	B	KEI SAITOU		JAP	6	AO6-TOO	TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009030/	Quick Look
176	AQL X-1	287.8264	0.5741	287.188103	0.49034	289.387425	22.822835	35.71314195	-4.15661165	244.5268	55855.5357986111	2011-10-21 12:51:33	55856.4599884259	2011-10-22 11:02:23	406010020	9.9406	40	10.041	9.9406	0	10.041	1	1	0	1	1	0	0	37.8451	37.8451	79.846	1	PROCESSED	57603.5073958333	2016-08-03 12:10:39	56241	2012-11-10 00:00:00	55873.3025578704	2011-11-08 07:15:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060036	We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object.	GALACTIC POINT SOURCES	4	A	KAZUTAKA YAMAOKA		JAP	6	AO6-TOO	SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406010020/	Quick Look
177	4U0114+65	19.4873	65.3067	18.650038	65.043652	51.171478	51.093575	125.69846298	2.57745686	71.642	55763.4307291667	2011-07-21 10:20:15	55764.9453472222	2011-07-22 22:41:18	406017010	106.4925	100	106.5508	106.5588	0	106.4925	2	2	0	2	1	0	0	88.5061	88.5061	130.8219	1	PROCESSED	57602.6518402778	2016-08-02 15:38:39	56152	2012-08-13 00:00:00	55785.0443981482	2011-08-12 01:03:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060071	We propose to observe an X-ray pulsar, 4U 0114+65 for 100 ks. This object is known to be a neutron star binary with an orbital period of 12 days and a long pulse priod of 10 ks. Our goals are to obtain time-averaged spectra of the XIS and HXD, and to quantify spectral changes between flare and quiescense phases, and to search for a cyclotron absorption line around ~ 60 keV. We also study pulse-phase resolved spectra. With these pieces of information, we aim at clarifying whether this source is a magnetar descendent or a neutron star with ordinary magnetic fields.	GALACTIC POINT SOURCES	4	A	MAKOTO SASANO		JAP	6	AO6	SEARCH FOR HIGH MAGNETIC NEUTRON STARS IN HIGH-MASS X-RAY BINARIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406017010/	Quick Look
178	EUVE J1439 +75.0	219.9459	75.0823	219.98134	75.295606	130.308915	72.229429	114.11249059	40.13551871	340.4897	56067.2884722222	2012-05-20 06:55:24	56067.8599421296	2012-05-20 20:38:19	407039010	29.9613	40	29.9693	29.9693	0	29.9613	1	1	0	1	1	0	0	32.3932	32.3932	49.3439	0	PROCESSED	57605.4757523148	2016-08-05 11:25:05	56442	2013-05-30 00:00:00	56076.028912037	2012-05-29 00:41:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070112	The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects.	GALACTIC POINT SOURCES	4	B	ATSUSHI HARAYAMA		JAP	7	AO7	SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407039010/	Quick Look
179	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
180	EXO 2030+375	308.0462	37.6555	307.574628	37.484842	325.998165	53.954312	77.15821576	-1.21997822	58.3113	56070.8420717593	2012-05-23 20:12:35	56072.789849537	2012-05-25 18:57:23	407089010	77.9451	75	77.9531	77.9569	0	77.9451	2	1	0	2	1	0	0	72.515	72.515	168.2558	0	PROCESSED	57605.5425347222	2016-08-05 13:01:15	56449	2013-06-06 00:00:00	56083.2088888889	2012-06-05 05:00:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072013	We propose to observe the Be/X-ray binary system EXO 2030+375 in the ascending part of one of its normal periastron flares for 75ks to study the onset of the pulsar activity. Quasi-periodic hour-long flux oscillations were recently observed during INTEGRAL serendipitous observations and by EXOSAT in 1985. They appear to happen at the viscous time-scale of a disk, evidencing some kind of instability in the transition zone between the magnetosphere and the accretion disk. The broad-band coverage and sensitivity of Suzaku will allow us to investigate in detail the opening of the magnetic gate for this high-magnetic field neutron star by studying the high time resolution light curve, the shape of its pulsed signal and the spectral properties.	GALACTIC POINT SOURCES	4	A	CARLO FERRIGNO		EUR	7	AO7	UNVEIL ACCRETION ONSET DURING A NORMAL OUTBURST OF EXO 2030+375	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407089010/	Quick Look
181	CRAB PULSAR	83.6302	22.0185	82.877911	21.9858	84.096687	-1.291934	184.55261516	-5.78447613	87.4628	56551.703599537	2013-09-16 16:53:11	56552.187650463	2013-09-17 04:30:13	408008010	0.2483	20	0.2483	0.2483	0	0.2483	2	2	0	2	1	0	0	16.312	16.312	41.8179	1	PROCESSED	57612.6349421296	2016-08-12 15:14:19	56956	2014-10-26 00:00:00	56588.603599537	2013-10-23 14:29:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080026	We hereby submit a proposal for Suzaku/HXD observations of the Crab pulsar' hard X-ray pulses, which will be coordinated with simultaneous detection of giant radio pulses at ground radio telescopes. With these observations, we will get a statistically significant confirmation (or denial) of the existence of correlation between X-ray intensity and giant radio pulses, which has been found, with a marginal significance, during our trial observations of the Crab pulsar in which we utilized the calibration data of the HXD. If this correlation is confirmed, a new insight into the physics of pulsars' magnetospheres can be obtained.	GALACTIC POINT SOURCES	4	C	TOSHIO TERASAWA		JAP	8	AO8	CORRELATION STUDY OF X-RAY PULSES AND GIANT RADIO PULSES FROM CRAB PULSAR WITH SUZAKU/HXD	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408008010/	Quick Look
182	ETA CARINAE	161.2758	-59.6779	160.789133	-59.414544	202.149273	-58.913486	287.59865979	-0.62113788	295.3343	56479.0480439815	2013-07-06 01:09:11	56481.2890509259	2013-07-08 06:56:14	408018020	83.9685	180	83.9685	83.9685	0	83.9685	2	2	0	2	1	0	0	75.7786	75.7786	193.6058	3	PROCESSED	57611.7548263889	2016-08-11 18:06:57	56861	2014-07-23 00:00:00	56492.6867361111	2013-07-19 16:28:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080081	Eta Carinae is a binary system containing two very massive main sequence stars orbiting with a period of 5.5 years. As reported by Sekiguchi et al. 2009 and Reitberger et al. 2012 based on Suzaku and Fermi data respectively, the system shows intense non-thermal emission extending from 20 keV to 200 GeV. Although detailed mechanism of this non-thermal emission has been clarified yet, it is now obvious that electrons and highly probably protons are accelerated to high energies by the collision of stellar winds. The aim of the present observation is to measure the spectral shape and flux of the non-thermal hard X-ray tail with the HXD, and compare with previous Suzaku observations. Based on a time variability (or non-variability), we examine proposed acceleration and emission mechanisms.	GALACTIC POINT SOURCES	4	B	TAKAYUKI YUASA		JAP	8	AO8	DETAILED SPECTROSCOPY OF NON-THERMAL HARD X-RAY EMISSION OF ETA CARINAE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408018020/	Quick Look
183	1RXSJ174559.6-370055	266.4961	-37.0139	265.645982	-36.994815	267.112271	-13.607714	353.13065719	-4.26083799	95.2535	57115.2722106482	2015-04-03 06:31:59	57115.6653240741	2015-04-03 15:58:04	409017010	14.2473	15	14.2473	14.2473	0	14.2633	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.9002777778	2016-08-17 21:36:24	57493	2016-04-15 00:00:00	57126.4170949074	2015-04-14 10:00:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090051	We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	B	HIDEYUKI MORI		JAP	9	AO9	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409017010/	Quick Look
184	GK PER	52.7957	43.9123	51.943474	43.742358	61.502929	24.084705	150.94865814	-10.09942696	88.9617	56876.7092708333	2014-08-07 17:01:21	56879.871712963	2014-08-10 20:55:16	409018010	109.7612	140	109.7612	114.4242	0	114.4722	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.4851157407	2016-08-16 11:38:34	57468	2016-03-21 00:00:00	56902.7320023148	2014-09-02 17:34:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090055	A 140-ks observation of the magnetic cataclysmic variable GK Per is proposed. By fitting Suzaku broadband spectra using our multitemperature spectral model of the accretion column, we estimate a white dwarf mass with statistical fitting errors smaller than 5%. The estimated mass will be compared with one obtained from the optical lightcurve fitting method developed and applied by Hachisu and Kato in a series of papers. GK Per is the only known magnetic cataclysmic variable which underwent classical nova explosion (in 1901), and both the mass estimation methods can be applied. Cross-validated WD mass estimation methods will be of importance in studying massive white dwarfs in accretion systems, in relation with the progenitor of type Ia supernovae.	GALACTIC POINT SOURCES	4	A	TAKAYUKI YUASA		JAP	9	AO9	CROSS VALIDATION OF WHITE DWARF MASS ESTIMATION METHODS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409018010/	Quick Look
185	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
186	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
187	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
188	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
189	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
190	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
191	CPD-28 2561	118.9748	-28.6234	118.467111	-28.489607	129.605392	-48.156505	245.44211654	-0.09136967	288.1635	56775.1365509259	2014-04-28 03:16:38	56775.9174768518	2014-04-28 22:01:10	409055010	26.9471	25	26.9471	26.9551	0	26.9631	2	2	0	2	1	0	0	23.1261	23.1261	67.4619	0	PROCESSED	57615.0079513889	2016-08-15 00:11:27	57214	2015-07-11 00:00:00	56848.6257638889	2014-07-10 15:01:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092005	We propose SUZAKU observations of the representative members of the class of magnetic massive O-type stars. The targets have measured magnetic fields and belong to similar spectral types. SUZAKU data will allow to compare the X-ray spectra of these objects that have similar stellar and wind parameters yet different magnetospheres. These observations will result in the first firm X-ray detections of our target stars. The analysis of XIS spectra will determine the emission measures and the temperatures of the hot gas. Our careful selection of targets will allow us to study the interplay between magnetic fields and stellar winds in O-type stars. These new observations for a comparative analysis of a homogeneous class of objects will be critical for driving the development of the theory.	GALACTIC POINT SOURCES	4	B	LIDIA OSKINOVA		EUR	9	AO9	COMPARATIVE STUDY OF MAGNETIC O-TYPE STARS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409055010/	Quick Look
192	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
193	U SCO	245.6292	-17.8133	244.907482	-17.696814	246.808074	3.687304	357.72295453	21.91020567	93.2753	55239.299224537	2010-02-12 07:10:53	55239.8259027778	2010-02-12 19:49:18	404018030	26.826	20	26.826	26.826	0	26.826	1	1	0	1	1	0	0	24.9037	24.9037	45.472	1	PROCESSED	57550.5610763889	2016-06-11 13:27:57	55619	2011-02-27 00:00:00	55253.1155671296	2010-02-26 02:46:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040057	We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each.	GALACTIC POINT SOURCES	4	A	DAI TAKEI		JAP	4	AO4-TOO	TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404018030/	Quick Look
194	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
195	XB1323-619	201.6454	-62.1418	200.814994	-61.88221	229.562797	-47.947963	307.02498182	0.45033402	99.5731	54109.4794907407	2007-01-09 11:30:28	54110.9168402778	2007-01-10 22:00:15	401002010	55.9368	50	55.9368	55.9368	0	55.9368	2	2	0	2	1	0	0	81.8173	81.8173	124.1769	1	PROCESSED	57536.8666087963	2016-05-28 20:47:55	54735	2008-09-26 00:00:00	54133.0271759259	2007-02-02 00:39:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010002	XB 1323-619 is a non-transient dipping LMXB and one of the few LMXB with spectrum extending to high energies. Our XMM-Newton observation revealed many lines including Fe XXV and XXVI absorption. Uniquely, the rate of bursting has increased systematically over 18 years by 15 times to every 20 min in 2006/07 making it the best source for study of absorption in bursts. Suzaku allows measurement of ADC temperature via the high energy cut-off and can give the first detection of cooling by soft photons from the neutron star from the change of cut-off energy during bursts. Curve-of-growth analysis gives the absorber temperature and tests our suggestion that absorption lines are formed in the ADC. Detailed comparison with burst theory is possible because of the regular bursting.	GALACTIC POINT SOURCES	4	C	TADAYASU DOTANI		JAP	1	AO1	BORADBAND INVESTIGATIONS OF THE DIPPING, BURSTGING LOW MASS X-RAY BINARY XB1323-619	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401002010/	Quick Look
196	HD45314	96.8131	14.89	96.098891	14.921299	96.656857	-8.393671	196.95740391	1.52274638	93.5296	56935.6339814815	2014-10-05 15:12:56	56937.7981134259	2014-10-07 19:09:17	409019010	82.0799	80	82.0879	82.0879	0	82.0799	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6300115741	2016-08-16 15:07:13	57355	2015-11-29 00:00:00	56989.5080208333	2014-11-28 12:11:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090079	We propose a Suzaku observation of a newly-found Gamma Cas analogue HD45314. The Gamma Cas analogues constitute a small but distinctive group showing anomalously hard X-ray spectra. We propose a Suzaku observation of HD45314 and compare it with the XMM data taken previously (Rauw et al. 2013) to reveal an expected change in the X-ray spectra. This will give us a clue to understand the X-ray production mechanism of this source and the gamma Cas analogues.	GALACTIC POINT SOURCES	4	B	MASAHIRO TSUJIMOTO		JAP	9	AO9	INVESTIGATION OF A GAMMA CAS ANALOGUES USING SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409019010/	Quick Look
197	HD110432	190.599	-63.0744	189.861553	-62.800339	224.074847	-51.705731	301.908501	-0.22062002	344.9423	54718.9065740741	2008-09-09 21:45:28	54719.7050231482	2008-09-10 16:55:14	403002010	25.3332	25	25.3332	25.3332	0	25.3332	2	2	0	2	1	0	0	21.3436	21.3436	68.9779	0	PROCESSED	57543.8037615741	2016-06-04 19:17:25	55148	2009-11-13 00:00:00	54780.4451736111	2008-11-10 10:41:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030005	We propose Suzaku observations of gamma Cas analogues. The sources in this class are characterized by extremely high thermal temperature and iron fluorescent line. We aim to identify the hard X-ray production site using the XIS's spectral capability at the iron K complex and the wide-band sensitivity combining XIS and HXD PIN.	GALACTIC POINT SOURCES	4	B	JUNICHIRO MIURA		JAP	3	AO3	SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403002010/	Quick Look
198	SGR1806-20	272.1595	-20.349	271.415501	-20.357687	272.017973	3.076639	10.0481975	-0.20823053	88.7483	54189.6305555556	2007-03-30 15:08:00	54190.0627199074	2007-03-31 01:30:19	401021010	19.2889	20	19.2889	19.595	0	19.3563	1	1	0	1	1	0	0	16.5071	16.5071	37.3279	1	PROCESSED	57538.0253587963	2016-05-30 00:36:31	54561	2008-04-05 00:00:00	54209.5169212963	2007-04-19 12:24:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010124	We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs.	GALACTIC POINT SOURCES	4	A	YUJIN NAKAGAWA		JAP	1	AO1-TOO	PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR"	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401021010/	Quick Look
199	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
200	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
201	EX HYA	193.0706	-29.2994	192.395685	-29.027802	203.848452	-21.746269	303.15288952	33.57198642	300.0004	54299.8912152778	2007-07-18 21:23:21	54302.4377199074	2007-07-21 10:30:19	402001010	100.5157	100	100.5237	100.5157	0	100.5237	2	2	0	2	1	0	0	91.1135	91.1135	219.9599	1	PROCESSED	57539.3319097222	2016-05-31 07:57:57	54707	2008-08-29 00:00:00	54339.5139467593	2007-08-27 12:20:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020008	The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS.	GALACTIC POINT SOURCES	4	A	MANABU ISHIDA		JAP	2	AO2	MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402001010/	Quick Look
202	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
203	PSR B1259-63	195.6782	-63.8867	194.888688	-63.618059	227.727553	-50.938083	304.17237227	-1.04211039	282.6534	54290.6852083333	2007-07-09 16:26:42	54291.1876041667	2007-07-10 04:30:09	402014020	19.4817	20	19.4817	19.4817	0	19.4817	2	2	0	2	1	0	0	26.9111	26.9111	43.378	1	PROCESSED	57539.1396759259	2016-05-31 03:21:08	54696	2008-08-18 00:00:00	54328.5032060185	2007-08-16 12:04:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014020/	Quick Look
204	PSR B1259-63	195.6089	-63.8685	194.820162	-63.599771	227.67155	-50.942181	304.14267075	-1.0226082	321.9333	54348.2308449074	2007-09-05 05:32:25	54348.6043287037	2007-09-05 14:30:14	402014080	18.3327	20	18.3407	18.3487	0	18.3327	1	1	0	1	1	0	0	22.3513	22.3513	32.26	0	PROCESSED	57539.9271412037	2016-05-31 22:15:05	54724	2008-09-15 00:00:00	54356.1999537037	2007-09-13 04:47:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014080/	Quick Look
205	HETEJ1900.1-2455	285.0506	-24.9802	284.284146	-25.050704	283.615122	-2.248458	11.25454685	-12.90928139	259.4192	54389.5913425926	2007-10-16 14:11:32	54390.5071064815	2007-10-17 12:10:14	402016010	41.7591	40	41.7788	41.7591	0	41.7751	2	2	0	2	1	0	0	39.9063	39.9063	79.1058	1	PROCESSED	57540.3158564815	2016-06-01 07:34:50	54771	2008-11-01 00:00:00	54403.1292708333	2007-10-30 03:06:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020068	We propose a 40 ks observation of the accreting millisecond pulsar HETE J1900.1-2455, which was discovered by HETE-2 only recently. Good sensitivity in 10-100keV and enough timing resolution of HXD on Suzaku allow us to measure the light curve and the phase resolved spectra of its hard X-ray pulsation, with which we study the physical parameters of the Comptonizing plasma that is considered as the source of the hard X-ray emission of accreting millisecond pulsars. With XIS, we study the radiation from the accretion disk and the neutron star surface, and search for spectral features such as emission lines or absorption edges, which will provide information on the binary environment.	GALACTIC POINT SOURCES	4	B	MOTOKO SUZUKI		JAP	2	AO2	HARD X-RAY PULSATION OF ACCRETION-DRIVEN MILLISECOND PULSAR HETE J1900.1-2455	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402016010/	Quick Look
206	TEVJ2032+4130	308.0461	41.5016	307.599311	41.330897	328.972015	57.41697	80.25613164	1.05964615	221.0839	54451.984212963	2007-12-17 23:37:16	54452.9176157407	2007-12-18 22:01:22	402031010	40.0439	40	40.0439	40.0439	0	40.0439	2	2	0	2	1	0	0	37.3091	37.3091	80.6419	1	PROCESSED	57540.8865625	2016-06-01 21:16:39	54828	2008-12-28 00:00:00	54460.6569675926	2007-12-26 15:46:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020150	Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku.	GALACTIC POINT SOURCES	4	C	SHUNJI KITAMOTO		JAP	2	AO2	STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402031010/	Quick Look
207	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
208	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
209	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
210	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
211	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
212	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
213	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
214	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
215	SAGITTARIUS A*	266.4146	-29.0061	265.619899	-28.986758	266.840195	-5.604294	359.94468967	-0.04360372	105.8159	57113.0215162037	2015-04-01 00:30:59	57113.6827662037	2015-04-01 16:23:11	409011050	28.6706	20	28.6706	28.6706	0	28.6866	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.891712963	2016-08-17 21:24:04	56748	2014-04-01 00:00:00	57125.4008796296	2015-04-13 09:37:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090048	With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	9	AO9	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011050/	Quick Look
216	EXO 0748-676	117.1051	-67.7525	117.068716	-67.625708	198.866436	-79.490243	279.97237585	-19.82332654	158.0884	54459.2369560185	2007-12-25 05:41:13	54460.2919444444	2007-12-26 07:00:24	402092010	45.8988	40	45.9126	45.8988	0	45.9046	2	2	0	2	1	0	0	43.5747	43.5747	91.1358	1	PROCESSED	57540.9732175926	2016-06-01 23:21:26	54854	2009-01-23 00:00:00	54483.1839351852	2008-01-18 04:24:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022014	We propose Suzaku observations of the dipping Low Mass X-ray Binaries (LMXBs) EXO 0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the absorbers and the HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components. This will allow to reliably determine the absolute values of the ionization parameters for each of the sources, which was not possible with XMM due to the lack of contemporaneous high energy spectra, providing for a detailed comparison of the absorbers with source properties such as luminosity.	GALACTIC POINT SOURCES	4	C	MARIA DIAZ TRIGO		EUR	2	AO2	BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402092010/	Quick Look
217	MARS-P8	103.1682	25.1356	102.40007	25.197197	101.91311	2.237602	190.38738197	11.42154102	298.1062	54559.9031365741	2008-04-03 21:40:31	54560.0072222222	2008-04-04 00:10:24	403006080	2.7489	100	2.7538	2.7578	0	2.7489	2	2	0	2	1	0	0	2.2864	2.2864	8.984	0	PROCESSED	57542.0500578704	2016-06-03 01:12:05	54953	2009-05-02 00:00:00	54577.1637615741	2008-04-21 03:55:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006080/	Quick Look
218	MARS-P20	103.6685	25.0732	102.900981	25.137167	102.37032	2.21732	190.63848879	11.80707935	298.2779	54560.9100347222	2008-04-04 21:50:27	54560.9932175926	2008-04-04 23:50:14	403006200	1.849	100	1.849	1.849	0	1.849	1	1	0	1	1	0	0	1.222	1.222	7.1839	0	PROCESSED	57542.0733101852	2016-06-03 01:45:34	54953	2009-05-02 00:00:00	54578.0575231482	2008-04-22 01:22:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006200/	Quick Look
219	MARS-P27	103.964	25.0399	103.196825	25.105264	102.640165	2.209619	190.78318678	12.0366945	298.3836	54561.4933217593	2008-04-05 11:50:23	54561.5418171296	2008-04-05 13:00:13	403006270	1.0998	100	1.1078	1.0998	0	1.1158	1	1	0	1	1	0	0	1.0935	1.0935	4.1839	0	PROCESSED	57542.2332175926	2016-06-03 05:35:50	54953	2009-05-02 00:00:00	54578.1251273148	2008-04-22 03:00:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006270/	Quick Look
220	RX J1712.6-2414	258.1492	-24.2444	257.386071	-24.185404	259.195725	-1.246505	359.8664305	8.74215246	94.4586	54889.4875925926	2009-02-27 11:42:08	54892.2710532407	2009-03-02 06:30:19	403021010	110.4813	100	110.4893	110.4813	0	110.4893	2	2	0	2	1	0	0	89.4584	89.4584	240.4418	4	PROCESSED	57545.7503587963	2016-06-06 18:00:31	55330	2010-05-14 00:00:00	54908.5588310185	2009-03-18 13:24:43	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030106	We propose to observe a peculiar Intermediate Polar, RX J1712.6-2414, which has no accretion disk around the white dwarf. This source shows the X-ray modulation only at the beat period and broad Fe-K emission lines in the phase-averaged spectrum. Our goal is to obtain a clear picture about the accretion flow geometry, which can explain the timing and spectral properties, utilizing the fine phase-resolved spectra. Furthermore, we examine the non-thermal emission from the source, since the magnetized white dwarf is a promising candidate of particle acceleration sites.	GALACTIC POINT SOURCES	4	B	HIDEYUKI MORI		JAP	3	AO3	ACCRETION FLOW AND EMISSION MECHANISM OF A DISKLESS INTERMEDIATE POLAR, RX J1712.6-2414	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403021010/	Quick Look
221	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
222	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
223	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
224	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
225	PSR J1429-5911	217.5051	-59.1899	216.584342	-58.967616	237.077372	-41.598198	315.26780851	1.30018252	101.124	55588.2265625	2011-01-27 05:26:15	55588.7001157407	2011-01-27 16:48:10	405012010	30.3824	30	30.3904	30.3984	0	30.3824	1	1	0	1	1	0	0	28.7923	28.7923	40.9039	0	PROCESSED	57600.7562384259	2016-07-31 18:08:59	55968	2012-02-11 00:00:00	55602.1404513889	2011-02-10 03:22:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050047	Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.	GALACTIC POINT SOURCES	4	C	NOBUYUKI KAWAI		JAP	5	AO5	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405012010/	Quick Look
226	ESO 137-G034	248.7664	-58.1298	247.710529	-58.026542	256.37198	-35.687232	329.07669192	-7.11373135	296.1293	54744.462650463	2008-10-05 11:06:13	54746.6745833333	2008-10-07 16:11:24	403075010	92.0525	90	92.0613	92.0587	0	92.0525	2	2	0	2	1	0	0	83.6615	83.6615	191.0897	1	PROCESSED	57544.095775463	2016-06-05 02:17:55	55148	2009-11-13 00:00:00	54780.6031828704	2008-11-10 14:28:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032025	Suzaku observations of hard X-ray (> 15 keV) selected, bright AGN discovered by INTEGRAL and Swift have revealed several examples of previously unknown Compton Thick (NH > 1e24 cm-2) AGN in the nearby Universe. Their broad band X-ray spectra show a high degree of complexity and a wide range of the relative intensities of the various components (i.e. scattered/reflected fraction; iron line intensity, etc.). We propose a medium/deep Suzaku observation of a bright source detected by INTEGRAL above 15 keV and optically identified with a nearby Seyfert 2 galaxy. Besides the various soft X-ray components, the flat 2-10 keV spectrum and the strong (EW ~ 1 keV) iron line present in an archival XMM-Newton observation strongly suggest that the nucleus is obscured by Compton-Thick gas.	GALACTIC POINT SOURCES	4	B	ROBERTO GILLI		EUR	3	AO3	ANOTHER COMPTON-THICK AGN JUST AROUND THE CORNER	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403075010/	Quick Look
227	BG CMI	112.8488	9.8847	112.163161	9.991257	113.00147	-11.750081	208.51997296	13.31865509	292.793	54932.5078703704	2009-04-11 12:11:20	54933.5710532407	2009-04-12 13:42:19	404029010	47.0791	40	47.0871	47.0791	0	47.0871	1	1	0	1	1	0	0	45.0346	45.0346	91.808	2	PROCESSED	57546.1223958333	2016-06-07 02:56:15	55324	2010-05-08 00:00:00	54949.5279050926	2009-04-28 12:40:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040113	We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.	GALACTIC POINT SOURCES	4	A	TAKAYUKI YUASA		JAP	4	AO4	SURVEY OBSERVATION OF INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404029010/	Quick Look
228	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
229	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
230	4U 1820-30	275.9267	-30.4234	275.123101	-30.450207	275.138047	-7.08832	2.73525617	-7.94773658	265.1815	55083.1120023148	2009-09-09 02:41:17	55083.2015740741	2009-09-09 04:50:16	404069010	3.5175	20	3.5255	3.5175	0	3.5255	1	1	0	1	1	0	0	3.7124	3.7124	7.738	0	PROCESSED	57548.5052546296	2016-06-09 12:07:34	55475	2010-10-06 00:00:00	55109.4203125	2009-10-05 10:05:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069010/	Quick Look
231	CYGNUS X-1	299.6653	35.165	299.194917	35.028212	313.740573	54.19441	71.33570459	2.99545336	212.8004	55182.0619328704	2009-12-17 01:29:11	55182.5508564815	2009-12-17 13:13:14	404075070	22.1019	300	22.1019	22.1099	0	23.664	1	1	0	1	1	0	0	3.4607	3.4607	42.236	0	PROCESSED	57549.8755671296	2016-06-10 21:00:49	54922	2009-04-01 00:00:00	55200.4490046296	2010-01-04 10:46:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075070/	Quick Look
232	CYGNUS X-1	299.6549	35.1555	299.184474	35.018756	313.721426	54.188323	71.32314713	2.99775182	222.7295	55173.647349537	2009-12-08 15:32:11	55174.1043287037	2009-12-09 02:30:14	404075200	20.0166	300	20.0166	21.7526	0	21.8593	1	1	0	1	1	0	0	17.4426	17.4426	39.4719	0	PROCESSED	57549.7233912037	2016-06-10 17:21:41	54922	2009-04-01 00:00:00	55189.2752430556	2009-12-24 06:36:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075200/	Quick Look
233	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
234	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
235	XSS J17223-7301	259.6949	-73.4263	258.137466	-73.372744	265.419963	-50.147658	319.10640118	-19.70481928	106.6643	55302.152650463	2010-04-16 03:39:49	55302.5939467593	2010-04-16 14:15:17	405033010	33.3861	30	33.3861	33.3861	0	33.3861	2	2	0	2	1	0	0	25.5889	25.5889	38.1279	0	PROCESSED	57551.2373726852	2016-06-12 05:41:49	55692	2011-05-11 00:00:00	55326.1437731482	2010-05-10 03:27:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050116	Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	5	AO5	QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405033010/	Quick Look
236	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
237	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
238	MU COL	86.4962	-32.3107	86.031401	-32.328862	84.748669	-55.688941	237.28985275	-27.10600903	93.5874	55455.752337963	2010-09-16 18:03:22	55456.3113541667	2010-09-17 07:28:21	405059010	25.961	20	25.961	25.961	0	25.961	1	1	0	1	1	0	0	21.8734	21.8734	48.2879	0	PROCESSED	57553.4381018518	2016-06-14 10:30:52	55836	2011-10-02 00:00:00	55469.2452314815	2010-09-30 05:53:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052005	We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models.	GALACTIC POINT SOURCES	4	A	LIDIA OSKINOVA		EUR	5	AO5	STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405059010/	Quick Look
239	4U 1909+07	287.7097	7.5883	287.10413	7.505006	290.320155	29.788203	41.89273161	-0.82371888	247.9131	55502.7037847222	2010-11-02 16:53:27	55503.4337731482	2010-11-03 10:24:38	405073010	29.2982	25	29.2982	29.2982	0	29.2982	2	2	0	2	1	0	0	21.3911	21.3911	63.0519	0	PROCESSED	57553.9348958333	2016-06-14 22:26:15	55882	2011-11-17 00:00:00	55515.2869328704	2010-11-15 06:53:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052024	We propose the first observation of the neutron star HMXB 4U 1909+07 with Suzaku. The aim of the proposed 25 ksec observation is to study the broadband spectrum of the source. The data will provide information about the structure and ionization state of the accreted medium, as well as of the geometry of the accretion column and the strength of the magnetic field. No high-resolution CCD spectra of this source have been published so far. The source shows flaring behavior, so the wind is expected to be strongly clumped, which could be probed by studying the evolution of N_H and the iron line with high time resolution. Furthermore we will perform phase resolved spectroscopy to study the spectral variation with pulse phase and perform a detailed search for a CRSF.	GALACTIC POINT SOURCES	4	A	FELIX FUERST		EUR	5	AO5	STUDYING ACCRETION IN THE UNCELEBRATED HMXB 4U 1909+07	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405073010/	Quick Look
240	AQL X-1	287.8278	0.5718	287.189492	0.488033	289.388601	22.82037	35.71173466	-4.15890942	243.2618	55858.7269328704	2011-10-24 17:26:47	55859.5786921296	2011-10-25 13:53:19	406010030	8.495	40	8.495	9.5383	0	9.5566	1	1	0	1	1	0	0	36.4768	36.4768	73.5819	2	PROCESSED	57603.6460416667	2016-08-03 15:30:18	56241	2012-11-10 00:00:00	55874.1380555556	2011-11-09 03:18:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060036	We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object.	GALACTIC POINT SOURCES	4	A	KAZUTAKA YAMAOKA		JAP	6	AO6-TOO	SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406010030/	Quick Look
241	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
242	OAO1657-415	255.2026	-41.6667	254.323073	-41.593508	258.36169	-18.820662	344.36019061	0.31327103	285.9012	55830.3988425926	2011-09-26 09:34:20	55832.6667939815	2011-09-28 16:00:11	406011010	84.7299	80	84.7337	84.7299	0	84.7417	2	2	0	2	1	0	0	74.5885	74.5885	195.9297	2	PROCESSED	57603.3220023148	2016-08-03 07:43:41	56226	2012-10-26 00:00:00	55858.2768518518	2011-10-24 06:38:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060037	We propose Suzaku observation of accretion-powered pulsar OAO 1657-415 to study matter accretion onto the neutron star. This object is a unique high mass X-ray binary (HMXB) that shows intermediate characteristics between wind-fed accretion pulsars and disk-fed accretion pulsars. High S/N spectra obtained by XIS, HXD-PIN/GSO with short exposure time (1 ks) allow us to investigate short-time variability of physical states of the accretion column, which is close to the neutron star surface. The proposed observation also reveals the matter distribution in the HMXB by using a 6.4-keV iron fluorescence line and hard X-rays. The data at the phase of eclipse egress provide essential information about the stellar wind and atmosphere of the companion star to constrain its stellar type in question.	GALACTIC POINT SOURCES	4	B	HIROKAZU ODAKA		JAP	6	AO6	WIDE-BAND X-RAY OBSERVATION OF HIGH MASS X-RAY BINARY PULSAR OAO 1657-415	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406011010/	Quick Look
243	1RXSJ175911.0-344921	269.7922	-34.8194	268.957803	-34.816359	269.8163	-11.378443	356.38251758	-5.46102238	72.1205	55993.9029513889	2012-03-07 21:40:15	55994.912650463	2012-03-08 21:54:13	406019010	40.1813	40	40.1813	40.1813	0	40.1813	2	2	0	2	1	0	0	34.751	34.751	87.2339	1	PROCESSED	57604.8358564815	2016-08-04 20:03:38	56385	2013-04-03 00:00:00	56016.6680787037	2012-03-30 16:02:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060085	We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test accretion disk theories at intermediate mass accretion rates.	GALACTIC POINT SOURCES	4	C	HIDEYUKI MORI		JAP	6	AO6	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406019010/	Quick Look
244	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
245	PSR B1259-63	195.6777	-63.8873	194.888189	-63.618658	227.727854	-50.938694	304.1721261	-1.04270018	282.6527	54292.6291319444	2007-07-11 15:05:57	54293.1910763889	2007-07-12 04:35:09	402014030	22.7217	20	22.7217	22.7217	0	22.7217	2	2	0	2	1	0	0	24.2808	24.2808	48.5459	0	PROCESSED	57539.1606712963	2016-05-31 03:51:22	54707	2008-08-29 00:00:00	54339.0273842593	2007-08-27 00:39:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014030/	Quick Look
246	IGR J16318-4848	247.9691	-48.8061	247.034981	-48.699533	253.953463	-26.583352	335.63186461	-0.44896472	266.5948	53961.4825	2006-08-14 11:34:48	53964.3488310185	2006-08-17 08:22:19	401094010	97.2538	100	97.2698	97.2538	97.2698	97.2698	2	2	2	2	1	0	0	87.1128	87.1128	247.6059	5	PROCESSED	57535.3483564815	2016-05-27 08:21:38	54526	2008-03-01 00:00:00	54020.9181597222	2006-10-12 22:02:09	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012034	We propose a detailed study of Compton thick X-ray absorption in neutral or weakly ionized material by using 100ksec of Suzaku observations of the strongly absorbed (N_H~2E24cm2) Galactic X-ray binary IGR J16318-4848. Measuring a high signal to noise ratio broad band spectrum will allow us to determine the curvature in the >10keV continuum caused by Compton downscattering in the absorber, to deduce its ionization state from observations of the Fe Kalpha line, and to study the variability of the source and the absorber. These observations will also shed more light onto the nature of the compact object in IGR J16318-4848.	GALACTIC POINT SOURCES	4	B	JOERN WILMS		EUR	1	AO1	OBSERVING IGR J16318-4848: PROBING COMPTON-THICK ABSORPTION	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401094010/	Quick Look
247	1RXSJ165256.3-264503	253.236	-26.7533	252.46137	-26.671186	255.025143	-4.179065	355.1420085	10.81079439	277.5876	54337.0024421296	2007-08-25 00:03:31	54338.0419444444	2007-08-26 01:00:24	402004010	49.5822	40	49.5822	49.5822	0	49.5822	2	2	0	2	1	0	0	46.6581	46.6581	89.7779	2	PROCESSED	57539.6777083333	2016-05-31 16:15:54	54723	2008-09-14 00:00:00	54350.4155092593	2007-09-07 09:58:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020015	We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, which were detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the Suzaku fine spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test acrretion disk theories at intermediate mass accretion rates.	GALACTIC POINT SOURCES	4	C	HIDEYUKI MORI		JAP	2	AO2	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402004010/	Quick Look
248	PSR B1259-63	195.6402	-63.8787	194.8511	-63.61001	227.698758	-50.941899	304.15600524	-1.03339065	289.9992	54315.2640856482	2007-08-03 06:20:17	54316.0419444444	2007-08-04 01:00:24	402014060	24.0388	20	24.0388	24.0388	0	24.0388	2	2	0	2	1	0	0	21.5808	21.5808	67.1959	1	PROCESSED	57539.3969675926	2016-05-31 09:31:38	54722	2008-09-13 00:00:00	54347.6946527778	2007-09-04 16:40:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014060/	Quick Look
249	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
250	4U 1543-624	236.9719	-62.5774	235.885471	-62.423392	250.451121	-41.357182	321.74901084	-6.34183385	299.1939	55826.4056828704	2011-09-22 09:44:11	55827.6217592593	2011-09-23 14:55:20	406072010	49.1851	50	49.1931	49.1851	0	49.2011	2	2	0	2	1	0	0	45.3094	45.3094	105.0599	1	PROCESSED	57603.2564699074	2016-08-03 06:09:19	56222	2012-10-22 00:00:00	55851.4556134259	2011-10-17 10:56:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062010	We propose to observe the ultra-compact X-ray binaries 4U 0614+091 and 4U 1543-624 for 50 ksec each. The aim of these observations is to constrain the inner radius of the accretion disc for both sources using the recently discovered in both sources relativistialy broadened OVIII Ly alpha line at ~0.7 keV. This constrains the radius of the neutron star. The second goal is to constrain the continuum using more physical model than was used in the literature so far. The unique, large energy coverage of Suzaku will enable us to break possible degeneracies between the properties of the broadened lines and the continuum, providing more convidence on the results.	GALACTIC POINT SOURCES	4	A	OLIWIA MADEJ		EUR	6	AO6	INVESTIGATING THE ORIGIN OF THE CONTINUUM AND LINE EMISSION IN THE UCXBS 4U 0614+091 AND 4U 1543-624	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406072010/	Quick Look
251	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
252	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
253	H1743-322	266.5662	-32.2338	265.750329	-32.21514	267.05149	-8.827747	357.25541352	-1.83396197	273.6881	56210.6462268518	2012-10-10 15:30:34	56211.5862731482	2012-10-11 14:04:14	407005020	21.1922	40	21.1922	21.1922	0	21.1922	3	2	0	2	1	0	0	41.517	41.517	81.2159	2	PROCESSED	57607.7447337963	2016-08-07 17:52:25	56595	2013-10-30 00:00:00	56226.5882291667	2012-10-26 14:07:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070002	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	7	AO7-TOO	MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407005020/	Quick Look
254	XTE J1855-206	283.8765	-2.601	283.223287	-2.666237	284.773693	20.130658	31.07954127	-2.09022498	75.074	57134.7127199074	2015-04-22 17:06:19	57137.3453125	2015-04-25 08:17:15	409022010	87.725	90	87.725	89.3274	0	89.3194	3	3	0	3	0	0	0	0	0	0	0	PROCESSED	57618.1026157407	2016-08-18 02:27:46	57593	2016-07-24 00:00:00	57224.4343171296	2015-07-21 10:25:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090101	Most of High mass X-ray binaries (HMXBs) have strong magnetic fields (~10^12 G) and detected cyclotron resonance scattering features (CRSFs). Many HMXBs with CRSFs have been observed by Suzaku and we derived a new method for estimating magnetic field strength using the observational data. In this observation, we try to observe candidates of strongly magnetized neutron star in HMXBs, EXO 1722-363 and XTE J1855-206 and examine the method.	GALACTIC POINT SOURCES	4	C	MAKOTO SASANO		JAP	9	AO9	EXAMINATION OF A NEW METHOD FOR ESTIMATING MAGNETIC FIELD STRENGTH WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409022010/	Quick Look
255	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
256	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
257	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
258	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
259	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
260	HEN 3-461	159.7779	-51.4088	159.258813	-51.147936	190.933881	-53.401362	282.90269516	6.2428626	116.1715	56278.1336342593	2012-12-17 03:12:26	56278.906400463	2012-12-17 21:45:13	407007010	45.7348	40	45.7348	45.7348	0	45.7348	2	2	0	2	1	0	0	46.6774	46.6774	66.7619	0	PROCESSED	57608.3071990741	2016-08-08 07:22:22	56018	2012-04-01 00:00:00	56303.5505902778	2013-01-11 13:12:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070021	Hard X-ray emitting symbiotic stars have been identified to emit 6.4 keV iron line with similar equivalent width of the 6.4 keV line of the Galactic Ridge X-ray Emission (GRXE). Only four of such hard X-ray emitting symbiotic stars have been observed with Suzaku. We propose to use Suzaku observations of all the eight newly discovered hard X-ray emitting symbiotic stars to ascertain if they have similar equivalent width of the 6.4 keV line of the GRXE. We will also confirm the emission of hard X-rays above 10 keV using the HXD PIN and use this feature to test for non-thermal emission in these objects.	GALACTIC POINT SOURCES	4	C	ROMANUS EZE		JAP	7	AO7	SEARCH FOR 6.4 KEV IRON EMISSION LINE IN THE NEWLY DISCOVERED HARD X-RAY EMITTING SYMBIOTIC STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407007010/	Quick Look
261	AX J1622.1-5005	245.5334	-50.0932	244.591386	-49.975777	252.45498	-28.129926	333.60606211	-0.20489946	274.3812	56160.9968402778	2012-08-21 23:55:27	56161.9398148148	2012-08-22 22:33:20	407018010	39.1263	40	40.5366	40.5366	0	39.1263	2	2	0	2	1	0	0	37.476	37.476	81.4619	0	PROCESSED	57606.9317824074	2016-08-06 22:21:46	56667	2014-01-10 00:00:00	56300.5637731482	2013-01-08 13:31:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070043	Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution.	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	7	AO7	ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407018010/	Quick Look
262	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
263	GX 339-4	255.7293	-48.7348	254.78204	-48.663918	259.585808	-25.807191	338.99236079	-4.30539701	107.9544	54915.3430555556	2009-03-25 08:14:00	54916.2711111111	2009-03-26 06:30:24	403011020	39.0792	40	39.1165	39.0792	0	39.1165	1	1	0	1	1	0	0	34.7852	34.7852	80.1658	0	PROCESSED	57545.909849537	2016-06-06 21:50:11	55330	2010-05-14 00:00:00	54930.1609490741	2009-04-09 03:51:46	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030046	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	3	AO3-TOO	MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403011020/	Quick Look
264	H1743-322	266.5676	-32.2352	265.751719	-32.216547	267.052722	-8.829118	357.25483145	-1.83570092	273.6877	56204.7822800926	2012-10-04 18:46:29	56205.6078240741	2012-10-05 14:35:16	407005010	20.811	40	20.811	20.811	0	20.811	2	2	0	2	1	0	0	42.4337	42.4337	71.3219	0	PROCESSED	57607.2960300926	2016-08-07 07:06:17	56595	2013-10-30 00:00:00	56226.5596296296	2012-10-26 13:25:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070002	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	7	AO7-TOO	MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407005010/	Quick Look
265	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
266	SGR 1806-20	272.1687	-20.4711	271.424026	-20.47983	272.024767	2.954425	9.94559743	-0.27498509	268.1397	54387.2332060185	2007-10-14 05:35:49	54388.333599537	2007-10-15 08:00:23	402094010	52.2477	50	52.2477	52.2717	0	52.2637	2	2	0	2	1	0	0	50.0895	50.0895	95.0599	1	PROCESSED	57540.2839583333	2016-06-01 06:48:54	54771	2008-11-01 00:00:00	54403.9548611111	2007-10-30 22:55:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022016	Among magnetars, SGR 1806-20 is particularly interesting since it emitted two years ago the most powerful giant flare ever observed. We are performing a long term monitoring in the soft X-rays with XMM-Newton and hard X-rays with INTEGRAL to study how the source evolves back to quiescence. We obtained in AO-1 a Suzaku observation that was carried out simultaneously with XMM-Newton and provided for the first time a broad band spectrum of SGR 1806-20 on a short timescale. A new observation is required to study the spectral variability in the hard X-ray range and possibly the properties of bursts.	GALACTIC POINT SOURCES	4	C	SANDRO MEREGHETTI		EUR	2	AO2	CONTINUED MONITORING OF SGR 1806-20 AFTER THE GIANT FLARE WITH SUZAKU AND XMM-NEWTON	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402094010/	Quick Look
267	1FGL J1018.6-5856	154.7461	-58.9386	154.30337	-58.687202	196.560422	-60.861111	284.35392298	-1.67969789	308.622	56105.7124189815	2012-06-27 17:05:53	56106.6523611111	2012-06-28 15:39:24	407096010	60.4324	60	60.4324	60.4324	0	60.4324	2	2	0	2	1	0	0	53.5978	53.5978	81.2059	1	PROCESSED	57606.5124768518	2016-08-06 12:17:58	56484	2013-07-11 00:00:00	56118.0496527778	2012-07-10 01:11:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	073113	Recently, a modulated signal has been detected with the Fermi from the source 1FGL J1018.6-5856. The presence of a O-type star in this source, and the variable character of the signal suggested that the source is a new gamma-ray binary system. Since it is expected that X-rays in these sources has the synchrotron origin, detailed X-ray observations are very important for understanding of the processes occurring in the system. However, sensitive observations of source in the X-ray energy bands are still missing. Therefore, we propose to observe the source with Suzaku. Since a long observational campaign is planned for 2012 by the HESS collaboration, the obtained X-ray, together with TeV, data will allow a proper modeling of the physical processes behind the non-thermal emission in system.	GALACTIC POINT SOURCES	4	B	HIROKAZU ODAKA	TAKAAKI TANAKA	JUS	7	AO7	X-RAY OBSERVATION OF GAMMA-RAY BINARY 1FGL J1018.6-5856	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407096010/	Quick Look
268	MARS-P5	103.045	25.1496	102.276729	25.210613	101.800688	2.241477	190.32670814	11.32616716	298.0638	54559.6600462963	2008-04-03 15:50:28	54559.7432407407	2008-04-03 17:50:16	403006050	1.9562	100	1.9562	1.9562	0	1.9562	2	2	0	2	1	0	0	1.9926	1.9926	7.1679	0	PROCESSED	57542.0421527778	2016-06-03 01:00:42	54953	2009-05-02 00:00:00	54577.1345486111	2008-04-21 03:13:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006050/	Quick Look
269	MARS-P9	103.2195	25.1275	102.451442	25.18934	101.960133	2.233755	190.41473742	11.46031922	298.1247	54560.0073726852	2008-04-04 00:10:37	54560.0766666667	2008-04-04 01:50:24	403006090	2.1506	100	2.1506	2.1746	0	2.1506	1	1	0	1	1	0	0	1.8919	1.8919	5.9759	0	PROCESSED	57542.0488888889	2016-06-03 01:10:24	54953	2009-05-02 00:00:00	54577.1428009259	2008-04-21 03:25:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006090/	Quick Look
270	V4641 SGR	274.8371	-25.4052	274.064433	-25.426808	274.361493	-2.037678	6.77442002	-4.78571714	84.0004	56741.9737152778	2014-03-25 23:22:09	56744.8959722222	2014-03-28 21:30:12	408002010	49.2237	100	49.2237	49.2706	0	49.2242	3	3	0	3	1	0	0	89.7439	89.7439	252.4556	1	PROCESSED	57614.1632291667	2016-08-14 03:55:03	57190	2015-06-17 00:00:00	56821.8685532407	2014-06-13 20:50:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080009	We propose a 100 ksec Suzaku observation of the Galactic microquasar V4641 Sgr in an outburst. V4641 Sgr has many unique charactersitics: 1)giant X-ray outbursts with fast rise and decay times, 2)violent variability in X-ray and optical bands, and 3)remarkable iron-K disk-line profiles in the X-ray spectrum. However, it is hardly understood due to the poor X-ray coverage which results from its short outburst duration and rapid intensity variations. Hence, we collaborate closely with VSNET, MAXI/GSC, Swift/XRT and Swift/BAT team for a rapid trigger. The moderate energy resolution and wideband energy coverage of Suzaku enable us to clarify the radiation mechanisms of V4641 Sgr. This observation is now planned simultaneously with Swift, many radio and optical/NIR observatories.	GALACTIC POINT SOURCES	4	A	KAZUTAKA YAMAOKA		JAP	8	AO8-TOO	THE LARGEST-EVER CAMPAIGN OF THE GALACTIC MICROQUASAR V4641 SGR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408002010/	Quick Look
271	MARS-P14	103.4188	25.1057	102.650967	25.168485	102.141964	2.228596	190.5119865	11.61511049	298.1941	54560.410150463	2008-04-04 09:50:37	54560.4933333333	2008-04-04 11:50:24	403006140	4.8252	100	4.8492	4.8252	0	4.8572	1	1	0	1	1	0	0	3.7214	3.7214	7.1759	0	PROCESSED	57542.063125	2016-06-03 01:30:54	54953	2009-05-02 00:00:00	54577.9434722222	2008-04-21 22:38:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006140/	Quick Look
272	MARS-P22	103.7541	25.0677	102.986656	25.132072	102.448087	2.219161	190.67657625	11.87528798	298.3117	54561.0767013889	2008-04-05 01:50:27	54561.1598842593	2008-04-05 03:50:14	403006220	4.0246	100	4.0406	4.0246	0	4.0476	1	1	0	1	1	0	0	4.102	4.102	7.1839	0	PROCESSED	57542.0781712963	2016-06-03 01:52:34	54953	2009-05-02 00:00:00	54578.0665625	2008-04-22 01:35:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006220/	Quick Look
273	4U 0614+091	94.2826	9.1348	93.597318	9.153924	94.364565	-14.241394	200.88027144	-3.36263018	270.7227	56737.0982291667	2014-03-21 02:21:27	56738.4584259259	2014-03-22 11:00:08	408009020	15.6689	60	15.8314	15.6689	0	15.8205	4	3	0	3	1	0	0	60.5574	60.5574	117.5018	2	PROCESSED	57614.0787152778	2016-08-14 01:53:21	57144	2015-05-02 00:00:00	56778.6809606482	2014-05-01 16:20:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080028	We propose an Suzaku observation of LMXB 4U 0614+091 for the study of Neutron Star Binary (NSB) in the low/hard state. An aim of this observation is to reveal a physical model of the NSB low/hard state in a same analogy of Black-Hole Binary (BHB) low/hard state. In the BHB Cyg X-1, the spectra in low/hard state radiate from a cool accretion disk and a hot comptonizing corona. A spectra of NS in low/hard state would have the same structure as Cyg X-1, but it is hard to study the fine structure of the spectra because of low luminosity. Suzaku can determine the low temperature of the disk and the high temperature of the corona, thanks to wide-band and high sensitivity detectors: XIS/BI and HXD. This observation is important for an unified model between BHB and NSB.	GALACTIC POINT SOURCES	4	B	SATOSHI SUGITA		JAP	8	AO8	THE SPECTRAL STUDY OF LMXB 4U 0614+091 IN THE LOW/HARD STATE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408009020/	Quick Look
274	HESS J0632+057	98.2456	5.8062	97.576893	5.844512	98.600946	-17.388931	205.66072349	-1.43796588	289.8173	54579.6856828704	2008-04-23 16:27:23	54580.6877199074	2008-04-24 16:30:19	403018010	44.076	40	44.076	44.076	0	44.076	2	2	0	2	1	0	0	41.4758	41.4758	86.5658	0	PROCESSED	57542.3746643518	2016-06-03 08:59:31	54961	2009-05-10 00:00:00	54594.1596990741	2008-05-08 03:49:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030080	We propose a 40 ks observation on HESS J0632+057, the newly discovered TeV gamma-ray source in the interacting region of Monoceros SNR and Rosette Nebula. Although this point-like source is found inside the error circle of an unidentified EGRET source 3EG J0634+0521, it has no clear counterpart at other wavelengths. Two sources, a weak X-ray source 1RXS J063258.3+05487 and a Be-star MCW 148, are found inside the error circle of HESS. The aim of the Suzaku observation is to obtain a clue to solve the yet feasible three scenarios of the TeV gamma-ray source.	GALACTIC POINT SOURCES	4	A	MOTOHIDE KOKUBUN		JAP	3	AO3	INVESTIGATION ON HESS J0632+057 IN MONOCEROS/ROSETTE REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403018010/	Quick Look
275	SAGITTARIUS A*	266.4166	-29.0014	265.621928	-28.982068	266.841834	-5.599552	359.94961276	-0.04264831	285.0058	56547.2597337963	2013-09-12 06:14:01	56547.6558101852	2013-09-12 15:44:22	408017020	19.276	20	19.2823	19.2901	0	19.276	3	3	0	3	1	0	0	21.0834	21.0834	34.218	0	PROCESSED	57612.6033796296	2016-08-12 14:28:52	56956	2014-10-26 00:00:00	56588.7462152778	2013-10-23 17:54:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017020/	Quick Look
276	ETA CARINAE	161.1825	-59.711	160.696763	-59.447791	202.133764	-58.970475	287.57247158	-0.67238651	329.3001	56476.1821296296	2013-07-03 04:22:16	56479.0417361111	2013-07-06 01:00:06	408018010	97.524	180	97.524	97.524	0	97.524	2	2	0	2	1	0	0	87.8367	87.8367	247.0497	2	PROCESSED	57611.768912037	2016-08-11 18:27:14	56861	2014-07-23 00:00:00	56492.7286921296	2013-07-19 17:29:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080081	Eta Carinae is a binary system containing two very massive main sequence stars orbiting with a period of 5.5 years. As reported by Sekiguchi et al. 2009 and Reitberger et al. 2012 based on Suzaku and Fermi data respectively, the system shows intense non-thermal emission extending from 20 keV to 200 GeV. Although detailed mechanism of this non-thermal emission has been clarified yet, it is now obvious that electrons and highly probably protons are accelerated to high energies by the collision of stellar winds. The aim of the present observation is to measure the spectral shape and flux of the non-thermal hard X-ray tail with the HXD, and compare with previous Suzaku observations. Based on a time variability (or non-variability), we examine proposed acceleration and emission mechanisms.	GALACTIC POINT SOURCES	4	B	TAKAYUKI YUASA		JAP	8	AO8	DETAILED SPECTROSCOPY OF NON-THERMAL HARD X-RAY EMISSION OF ETA CARINAE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408018010/	Quick Look
277	V2301 OPH	270.155	8.1565	269.554142	8.157196	270.169577	31.596745	34.53366867	14.97765204	262.0679	56576.0003009259	2013-10-11 00:00:26	56577.3452314815	2013-10-12 08:17:08	408024020	53.1884	110	53.1884	53.1884	0	53.1884	2	2	0	2	1	0	0	47.2892	47.2892	116.1898	0	PROCESSED	57612.9583333333	2016-08-12 23:00:00	57184	2015-06-11 00:00:00	56631.6754282407	2013-12-05 16:12:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080107	It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion.	GALACTIC POINT SOURCES	4	A	TAKAYUKI HAYASHI		JAP	8	AO8	MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408024020/	Quick Look
278	V2301 OPH	270.1437	8.1764	269.542941	8.17715	270.156471	31.616658	34.54710657	14.99643028	71.9008	56752.9922800926	2014-04-05 23:48:53	56754.6945949074	2014-04-07 16:40:13	408024030	62.9253	57	62.9413	62.9253	0	62.9413	2	2	0	2	1	0	0	56.5037	56.5037	147.0677	1	PROCESSED	57614.2091666667	2016-08-14 05:01:12	57184	2015-06-11 00:00:00	56817.8149884259	2014-06-09 19:33:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080107	It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion.	GALACTIC POINT SOURCES	4	A	TAKAYUKI HAYASHI		JAP	8	AO8	MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408024030/	Quick Look
279	WR140	305.1942	43.809	304.771615	43.649401	327.418451	60.430238	80.92425741	4.10518752	220.5408	54812.4360069444	2008-12-12 10:27:51	54813.5523148148	2008-12-13 13:15:20	403032010	52.9106	40	52.9106	52.9106	0	52.9106	3	3	0	3	1	0	0	48.2609	48.2609	96.4318	0	PROCESSED	57544.9612847222	2016-06-05 23:04:15	55192	2009-12-27 00:00:00	54826.2481365741	2008-12-26 05:57:19	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030157	WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	3	AO3	X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403032010/	Quick Look
280	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
281	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
282	X 1630-472	248.5011	-47.3955	247.580071	-47.291357	254.086008	-25.133666	336.90685721	0.25132488	88.6334	57080.103125	2015-02-27 02:28:30	57081.1542824074	2015-02-28 03:42:10	409007030	5.1108	40	5.128	5.1452	0	5.1108	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.7393634259	2016-08-17 17:44:41	57458	2016-03-11 00:00:00	57091.4579513889	2015-03-10 10:59:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090015	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	9	AO9-TOO	MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409007030/	Quick Look
283	SAGITTARIUS A*	266.415	-29.0091	265.620279	-28.98976	266.840621	-5.607284	359.94231116	-0.0454652	105.8502	57103.3174537037	2015-03-22 07:37:08	57103.7690162037	2015-03-22 18:27:23	409011040	23.2422	20	23.2422	23.2465	0	23.2465	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.8342824074	2016-08-17 20:01:22	56748	2014-04-01 00:00:00	57114.6078472222	2015-04-02 14:35:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090048	With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	9	AO9	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011040/	Quick Look
284	1RXSJ013106.4+612035	22.7619	61.3591	21.928492	61.101677	49.598028	47.010357	127.66105316	-1.14841945	76.8129	55765.7032175926	2011-07-23 16:52:38	55766.0182060185	2011-07-24 00:26:13	406034010	13.2963	20	13.2963	13.2963	0	13.2963	1	1	0	1	1	0	0	15.8829	15.8829	27.1999	0	PROCESSED	57602.6424884259	2016-08-02 15:25:11	56374	2013-03-23 00:00:00	55784.9886458333	2011-08-11 23:43:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060097	We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray.	GALACTIC POINT SOURCES	4	B	HIROMITSU TAKAHASHI		JAP	6	AO6	SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406034010/	Quick Look
285	1RXSJ173916.2-214746	264.8155	-21.7912	264.064028	-21.764222	265.175612	1.563021	5.33311568	4.97377326	96.7097	57115.0060069444	2015-04-03 00:08:39	57115.2681712963	2015-04-03 06:26:10	409015010	12.328	12	12.349	12.3523	0	12.328	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8972800926	2016-08-17 21:32:05	57493	2016-04-15 00:00:00	57126.415625	2015-04-14 09:58:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090051	We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	B	HIDEYUKI MORI		JAP	9	AO9	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409015010/	Quick Look
286	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
287	UX ARIETIS	51.6466	28.6421	50.887812	28.467932	56.479497	9.555722	159.59610539	-22.97107378	272.6966	55229.7116666667	2010-02-02 17:04:48	55231.7321064815	2010-02-04 17:34:14	404008010	87.7993	90	87.7993	87.7993	0	87.7993	2	2	0	2	1	0	0	79.7429	79.7429	174.5399	0	PROCESSED	57550.5166203704	2016-06-11 12:23:56	55616	2011-02-24 00:00:00	55249.830150463	2010-02-22 19:55:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040036	We propose a hard X-ray observation of RS CVn-type active binary UX Arietis. Detection of nonthermal hard X-ray radiation is essentially important to solve the generation mechanism of stellar flares. UX Ari has a high coronal activity with a high temperature of ~2keV, and large stellar flares were frequently observed in the radio, UV, and X-ray band. Therefore, UX Ari is very suitable for hard X-ray observation of stellar flares. Large X-ray flares were observed by BeppoSAX, ASCA and Ginga sattellite, and hard X-ray emission upto ~50keV is detected by BeppoSAX. If a flare is large such as the events of former X-ray observations, we can detect the nonthermal hard X-ray emssion by Suzaku HXD.	GALACTIC POINT SOURCES	4	C	SHIN-NOSUKE ISHIKAWA		JAP	4	AO4	STUDY ON GENERATION MECHANISM OF STELLAR FLARES BY HARD X-RAY OBSERVATION OF ACTIVE BINARY UX ARIETIS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404008010/	Quick Look
288	HESS J0632+057	98.2448	5.8057	97.576095	5.844008	98.600145	-17.389477	205.66080027	-1.43890266	289.9631	54941.5631944444	2009-04-20 13:31:00	54944.1542708333	2009-04-23 03:42:09	404027010	100.0343	100	100.0343	100.0343	0	100.0343	2	2	0	2	1	0	0	82.3918	82.3918	223.8419	6	PROCESSED	57546.2406481482	2016-06-07 05:46:32	55336	2010-05-20 00:00:00	54966.5323958333	2009-05-15 12:46:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040102	We propose a coordinate observation of HESS J0632+057 with Suzaku and VLA. This source is recently discovered as a fourth gamma-ray binary with HESS and XMM-Newton, and our results obtained in Suzaku AO-3 also confirmed a gradual variety of X-ray intensity, possibly associated with the binary period. With a combined observation with VLA, we will for the first time obtain a "real-time" variety from both of image and spectrum of this interesting source.	GALACTIC POINT SOURCES	4	A	MOTOHIDE KOKUBUN		JAP	4	AO4	SIMULTANEOUS OBSERVATION OF HESS J0632+057 WITH SUZAKU AND VLA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404027010/	Quick Look
289	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
290	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
291	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
292	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
293	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
294	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
295	4U 1820-30	275.9314	-30.4193	275.127829	-30.44613	275.142299	-7.084391	2.74079847	-7.94949913	261.8762	55102.6696759259	2009-09-28 16:04:20	55103.5002662037	2009-09-29 12:00:23	404069040	28.6994	20	28.6994	28.6994	0	28.6994	3	2	0	3	1	0	0	24.9261	24.9261	71.7519	2	PROCESSED	57548.6752546296	2016-06-09 16:12:22	55499	2010-10-30 00:00:00	55133.2273263889	2009-10-29 05:27:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069040/	Quick Look
296	1E 2259+586	345.2716	58.9493	344.749816	58.680435	23.84389	56.952455	109.11022544	-0.92895504	86.3239	54976.8335300926	2009-05-25 20:00:17	54978.6446064815	2009-05-27 15:28:14	404076010	122.5791	120	122.5809	122.5809	0	122.5791	2	2	0	2	1	0	0	103.4462	103.4462	156.4638	1	PROCESSED	57546.7298726852	2016-06-07 17:31:01	54922	2009-04-01 00:00:00	54992.6935069444	2009-06-10 16:38:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	4	AO4	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404076010/	Quick Look
297	CYGNUS X-1	299.5891	35.272	299.119523	35.135533	313.701858	54.316122	71.39464341	3.10435878	91.3113	54935.7650462963	2009-04-14 18:21:40	54936.1473958333	2009-04-15 03:32:15	404075030	17.1088	300	17.1088	17.1168	0	17.1088	2	1	0	2	1	0	0	12.986	12.986	33.0279	1	PROCESSED	57546.1452662037	2016-06-07 03:29:11	54922	2009-04-01 00:00:00	54949.5303240741	2009-04-28 12:43:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075030/	Quick Look
298	V1280 SCO	254.4172	-32.3368	253.607248	-32.260102	256.681689	-9.612724	351.33470039	6.5596985	97.7451	55605.3662615741	2011-02-13 08:47:25	55608.0501851852	2011-02-16 01:12:16	405029010	99.683	100	99.699	99.683	0	99.699	2	2	0	2	1	0	0	86.9306	86.9306	231.8739	2	PROCESSED	57600.9978472222	2016-07-31 23:56:54	55983	2012-02-26 00:00:00	55617.4142361111	2011-02-25 09:56:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050110	We propose a 100 ks observation of the C-rich classical nova V1280 Sco. Using Suzaku's excellent spectral performance in the soft X-ray energy band, we aim to detect and to resolve emission lines from C, N, and O.	GALACTIC POINT SOURCES	4	A	DAI TAKEI		JAP	5	AO5	X-RAY SPECTROSCOPY OF THE C-RICH CLASSICAL NOVA V1280 SCO	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405029010/	Quick Look
299	CYGNUS X-1	299.6021	35.1308	299.131607	34.994279	313.637751	54.179562	71.27949874	3.02171591	263.2299	55125.3772106482	2009-10-21 09:03:11	55125.8404398148	2009-10-21 20:10:14	404075130	20.4985	300	20.4985	20.5065	0	20.4985	2	1	0	2	1	0	0	15.163	15.163	40.0159	0	PROCESSED	57548.9405208333	2016-06-09 22:34:21	54922	2009-04-01 00:00:00	55134.2701967593	2009-10-30 06:29:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075130/	Quick Look
300	CYGNUS X-1	299.6206	35.1339	299.150096	34.997301	313.663881	54.177403	71.29004535	3.01042005	252.1788	55138.8946180556	2009-11-03 21:28:15	55139.4106365741	2009-11-04 09:51:19	404075150	22.6168	300	22.6168	22.6248	0	22.6168	2	1	0	2	1	0	0	14.061	14.061	44.5759	1	PROCESSED	57549.0593981482	2016-06-10 01:25:32	54922	2009-04-01 00:00:00	55149.4202199074	2009-11-14 10:05:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075150/	Quick Look
301	24M2791	334.9577	63.2629	334.551329	63.011149	23.890285	63.530312	106.81877019	5.23758822	230.0008	55947.3704513889	2012-01-21 08:53:27	55948.0926388889	2012-01-22 02:13:24	406023010	34.6017	30	34.6177	34.6017	0	34.6097	2	2	0	2	1	0	0	35.0595	35.0595	62.3919	0	PROCESSED	57604.5087847222	2016-08-04 12:12:39	56340	2013-02-17 00:00:00	55973.1102893518	2012-02-16 02:38:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060087	We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object.	GALACTIC POINT SOURCES	4	C	MASANORI OHNO		JAP	6	AO6	SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406023010/	Quick Look
302	PSR J0614-33	93.5386	-33.5015	93.081964	-33.485438	95.411067	-56.876431	240.50300829	-21.83180137	119.1484	55498.9719675926	2010-10-29 23:19:38	55499.6140740741	2010-10-30 14:44:16	405014010	31.2109	30	31.2109	31.2109	0	31.2109	2	2	0	2	1	0	0	27.3314	27.3314	55.4499	0	PROCESSED	57553.8985763889	2016-06-14 21:33:57	55875	2011-11-10 00:00:00	55509.0359722222	2010-11-09 00:51:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050047	Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.	GALACTIC POINT SOURCES	4	C	NOBUYUKI KAWAI		JAP	5	AO5	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405014010/	Quick Look
303	EMS0918	211.2948	-61.3938	210.393622	-61.154695	234.671242	-44.951341	311.64055354	0.22486043	106.822	55589.5588310185	2011-01-28 13:24:43	55590.0834837963	2011-01-29 02:00:13	405025010	24.5425	20	24.5505	24.5425	0	24.5585	2	2	0	2	1	0	0	23.2811	23.2811	45.3099	1	PROCESSED	57600.7734606482	2016-07-31 18:33:47	55972	2012-02-15 00:00:00	55602.2015046296	2011-02-10 04:50:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050104	Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV.	GALACTIC POINT SOURCES	4	A	YASUYUKI TANAKA		JAP	5	AO5	SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405025010/	Quick Look
304	EMS1308	293.0393	19.2567	292.487947	19.148974	299.013622	40.405253	54.62289289	0.10827332	90.0001	55313.4365740741	2010-04-27 10:28:40	55313.9766203704	2010-04-27 23:26:20	405028010	23.8987	20	23.9067	23.9067	0	23.8987	3	2	0	2	1	0	0	23.209	23.209	46.652	1	PROCESSED	57551.306400463	2016-06-12 07:21:13	55693	2011-05-12 00:00:00	55327.1789930556	2010-05-11 04:17:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050104	Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV.	GALACTIC POINT SOURCES	4	A	YASUYUKI TANAKA		JAP	5	AO5	SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405028010/	Quick Look
305	CYG X-1	299.5787	35.2024	299.108699	35.065978	313.648056	54.25343	71.3307159	3.0753508	59.5691	56419.0925578704	2013-05-07 02:13:17	56419.6071643518	2013-05-07 14:34:19	407015020	1.5124	20	3.2442	1.5124	0	21.48	2	2	0	1	1	0	0	20.9258	20.9258	44.458	0	PROCESSED	57611.2625347222	2016-08-11 06:18:03	56808	2014-05-31 00:00:00	56442.9715509259	2013-05-30 23:19:02	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070030	We propose to observe Cyg X-1 for 85 ks, utilizing P-sum mode for XIS3. Our aim is to perform shot analysis, which is originally invented by Negoro et al. 1995 with Ginga, and obtain high-quality wide-band spectra for several phases in less than 1 sec; for example, 0.1 sec before the peak, +/- 0.05 sec at the peak, and after the peak. With these spectra, we will quantify changes in five spectral components: hard Comptonization, soft Comptonization, disk emission, Fe-K lines, and reflection. This will be a clue to know long-standing mystery on rapid variability in black holes.	GALACTIC POINT SOURCES	4	A	SHINYA YAMADA		JAP	7	AO7	INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407015020/	Quick Look
306	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
307	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
308	HER X-1	254.4619	35.2659	254.010863	35.341503	246.021498	57.41824	58.05460857	37.50723847	268.3041	55461.7937037037	2010-09-22 19:02:56	55462.2467476852	2010-09-23 05:55:19	405058040	21.74	20	21.74	21.796	0	21.8704	1	1	0	1	1	0	0	19.803	19.803	39.1359	0	PROCESSED	57553.5121180556	2016-06-14 12:17:27	55840	2011-10-06 00:00:00	55474.0995486111	2010-10-05 02:23:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052001	We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity?	GALACTIC POINT SOURCES	4	B	R DIGER STAUBERT		EUR	5	AO5	VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405058040/	Quick Look
309	GX 339-4	255.7013	-48.7851	254.753538	-48.714085	259.571516	-25.859202	338.94105066	-4.32130146	91.6296	55620.1778703704	2011-02-28 04:16:08	55620.8022569445	2011-02-28 19:15:15	405063040	21.799	20	21.799	21.807	0	21.8168	3	3	0	3	1	0	0	18.8502	18.8502	53.9239	0	PROCESSED	57601.0624074074	2016-08-01 01:29:52	56009	2012-03-23 00:00:00	55642.1310300926	2011-03-22 03:08:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052015	We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4	GALACTIC POINT SOURCES	4	A	CLEMENT CABANAC		EUR	5	AO5-TOO	PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063040/	Quick Look
310	1RXS J1708-4009	257.2038	-40.2142	256.334135	-40.15046	259.790997	-17.224743	346.43162325	-0.00870489	267.1357	55466.6124074074	2010-09-27 14:41:52	55467.7738425926	2010-09-28 18:34:20	405076010	62.8109	60	62.8189	62.8226	0	62.8109	3	2	0	2	1	0	0	59.5114	59.5114	100.3239	1	PROCESSED	57553.5661342593	2016-06-14 13:35:14	55287	2010-04-01 00:00:00	55477.2762268518	2010-10-08 06:37:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	5	AO5	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405076010/	Quick Look
311	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
312	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
313	4U 1705-44	257.2257	-44.096	256.322601	-44.032282	260.19112	-21.088012	343.32512852	-2.33758895	104.9955	56013.5320486111	2012-03-27 12:46:09	56016.4231134259	2012-03-30 10:09:17	406076010	100.8112	100	100.8112	100.8192	0	100.8209	2	2	0	2	1	0	0	90.0759	90.0759	249.7677	2	PROCESSED	57605.1022453704	2016-08-05 02:27:14	56393	2013-04-11 00:00:00	56027.2013657407	2012-04-10 04:49:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062019	We propose a ToO Suzaku 100-ks observation of the neutron star X-ray binary 4U 1705-44, to perform a detailed study of its broad-band (0.4-200 keV) X-ray spectrum during a hard state. XIS data will provide important information on the iron K-shell features, and the broad-band spectral capabilities of the HXD will allow to study the hard X-ray spectrum and in particular the Compton reflection bump at 20-50 keV. We plan to fit both the iron features and the reflection bump with a self-consistent model, which will allow to prove (or disprove) a disk origin of the iron line. Moreover the proposed observation will allow to study the correlation between the spectral index of the primary spectrum and the reflection amplitude, which gives important constraints on the geometry of the system.	GALACTIC POINT SOURCES	4	A	TIZIANA DI SALVO		EUR	6	AO6-TOO	SUZAKU BROAD-BAND OBSERVATION OF 4U 1705-44: PROBING THE DISK ORIGIN OF THE IRON LINE IN THE HARD STATE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406076010/	Quick Look
314	SAGITTARIUS A*	266.415	-29.0052	265.620304	-28.98586	266.840523	-5.603385	359.94564014	-0.04343346	106.9998	56738.4724189815	2014-03-22 11:20:17	56738.9897685185	2014-03-22 23:45:16	408017070	21.5887	20	21.6185	21.5887	0	21.6442	2	2	0	2	1	0	0	19.274	19.274	44.694	0	PROCESSED	57614.0833680556	2016-08-14 02:00:03	57120	2015-04-08 00:00:00	56750.8212268518	2014-04-03 19:42:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017070/	Quick Look
315	1RXSJ170047.8-314442	255.196	-31.7452	254.389249	-31.672155	257.283531	-8.954733	352.21229356	6.40020757	90.7944	56341.4932060185	2013-02-18 11:50:13	56341.7501273148	2013-02-18 18:00:11	407027010	8.9262	12	8.9262	8.9262	0	8.9262	2	2	0	2	1	0	0	8.232	8.232	22.186	0	PROCESSED	57610.6225810185	2016-08-10 14:56:31	56718	2014-03-02 00:00:00	56352.4986458333	2013-03-01 11:58:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070052	We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	C	HIDEYUKI MORI		JAP	7	AO7	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407027010/	Quick Look
316	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
317	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
318	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
319	FS AURIGAE	86.945	28.5962	86.152995	28.579446	87.308718	5.183997	180.53629966	0.22811281	90.5955	56541.1879050926	2013-09-06 04:30:35	56542.802974537	2013-09-07 19:16:17	408041010	62.1842	62	62.1842	62.1842	0	62.1842	2	2	0	2	1	0	0	61.0287	61.0287	139.5158	0	PROCESSED	57612.5675810185	2016-08-12 13:37:19	56981	2014-11-20 00:00:00	56616.7165046296	2013-11-20 17:11:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082012	FS Aur represents one of the most unusual cataclysmic variable to have ever been observed. It is famous for a variety of uncommon and puzzling periodic photometric and spectroscopic variabilities. Tovmassian, Zharikov & Neustroev (2007) proposed that the precession of a fast-rotating magnetically accreting white dwarf can successfully explain these phenomena. We request 62 ks observations of FS Aur to detect the magnetic WD, determine its spin period, confirm the flux and spectral variability with the precession period, inconclusively detected by Chandra and Swift, and thus to check the proposed model. The theory of compact objects predicts certain relations between the spin and precession periods, and our findings will provide a good test for the theory.	GALACTIC POINT SOURCES	4	B	VITALY NEUSTROEV		EUR	8	AO8	PROBING THE PRECESSION OF WHITE DWARF IN CLOSE BINARY SYSTEMS - FS AURIGAE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408041010/	Quick Look
320	4U 1735-44	264.7398	-44.4536	263.827347	-44.425856	265.968173	-21.085622	346.05003995	-6.99385769	96.4379	57098.6918402778	2015-03-17 16:36:15	57099.2717824074	2015-03-18 06:31:22	408043030	4.3665	20	4.3665	4.9159	0	4.967	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8209027778	2016-08-17 19:42:06	57479	2016-04-01 00:00:00	57112.402662037	2015-03-31 09:39:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082017	We propose to observe the bursting low-mass X-ray binary 4U 1735-44 with Suzaku for a total exposure time of 60 ks. We plan to investigate the broad-band X-ray spectrum by performing a detailed spectroscopic and timing analysis in the energy range 0.4-100 keV. The main scientific aims of this observation are to detect and study the iron Kalpha line at 6.4-7 keV, simultaneously with the expected iron edge at 7-9 keV, emission lines at lower energy (such as S, Ar and Ca at 2.62 keV, 3.31 keV and 3.90 keV, respectively), and either a Compton reflection hump at 20-40 keV or a hard tail at energy above 25 keV (depending of the state of the source), thanks to the broad-band capabilities of Suzaku. This will allow to infer and probe the origin of these components, which is still debated.	GALACTIC POINT SOURCES	4	A	ELISE EGRON		EUR	8	AO8	BROAD-BAND SPECTRAL ANALYSIS AND STUDY OF THE DISK REFLECTION COMPONENT IN 4U 1735-44 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408043030/	Quick Look
321	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
322	JUPITER	226.6349	-16.1983	225.936085	-16.00589	228.727521	1.247844	344.01962259	35.67652355	118.4908	53793.86	2006-02-27 20:38:24	53794.9585532407	2006-02-28 23:00:19	401001040	42.2558	36	42.2638	42.2638	42.2638	42.2558	2	2	2	2	1	0	0	35.7067	35.7067	94.9059	2	PROCESSED	57533.1103819444	2016-05-25 02:38:57	54401	2007-10-28 00:00:00	53906.5712615741	2006-06-20 13:42:37	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011003	We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure.	GALACTIC POINT SOURCES	4	C	RONALD ELSNER		USA	1	AO1	JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001040/	Quick Look
323	4U 1705-44	257.2313	-44.1028	256.328133	-44.039108	260.196098	-21.094402	343.32206131	-2.34487049	297.0793	54014.4242708333	2006-10-06 10:10:57	54015.0891087963	2006-10-07 02:08:19	401046030	20.065	20	20.065	20.065	20.065	20.065	2	2	2	2	1	0	0	17.9196	17.9196	57.4239	2	PROCESSED	57535.7945138889	2016-05-27 19:04:06	54526	2008-03-01 00:00:00	54021.6765162037	2006-10-13 16:14:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011112	We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state.	GALACTIC POINT SOURCES	4	A	ANDREW YOUNG		USA	1	AO1	REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046030/	Quick Look
324	GX 339-4	255.7025	-48.7916	254.754666	-48.72059	259.573177	-25.865576	338.93635594	-4.32587966	86.7489	54143.2316087963	2007-02-12 05:33:31	54146.2003009259	2007-02-15 04:48:26	401068010	77.2053	100	83.8935	77.2053	0	82.1138	2	2	0	2	1	0	0	94.026	94.026	256.484	4	PROCESSED	57537.4905208333	2016-05-29 11:46:21	54535	2008-03-10 00:00:00	54167.7751851852	2007-03-08 18:36:16	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011146	Skewed iron emission lines from the inner accretion disk and broad-band disk reflection spectra are incisive diagnostics of relativistic effects and the inner accretion flow geometry in black hole binaries. With its high effective area, efficient instrument modes, and sensitivity in hard X-rays, Suzaku is ideally suited to fully exploit these diagnostics. We request a total of 154 ksec in up to four observations to observe a black hole transient in outburst, using a scheme tailored to accommodate different source fluxes and Suzaku's observing windows. We will support these observations with a global multi-wavelength network of observatories. Understanding accretion onto black holes is central to NASA's ``SEU'' research theme.	GALACTIC POINT SOURCES	4	A	JON MILLER		USA	1	AO1-TOO	SUZAKU OBSERVATIONS OF A BLACK HOLE TRANSIENT IN OUTBURST	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401068010/	Quick Look
325	RS OPH	267.5535	-6.6951	266.880129	-6.681587	267.45304	16.723864	19.81011082	10.37967032	94.9072	55987.2608796296	2012-03-01 06:15:40	55988.855	2012-03-02 20:31:12	406033010	69.386	100	69.386	69.386	0	69.386	2	2	0	2	1	0	0	60.0899	60.0899	137.7198	0	PROCESSED	57604.8300810185	2016-08-04 19:55:19	56375	2013-03-24 00:00:00	56008.324224537	2012-03-22 07:46:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060096	We propose a 100 ks observation of a recurrent novae remnant RS Ophiuchi. Using Suzaku's wide-energy coverage and excellent spectral performance, we aim to diagnose plasma and to discover non-thermal emission at a recurrent novae remnant.	GALACTIC POINT SOURCES	4	C	DAI TAKEI		JAP	6	AO6	OBSERVATION OF A RECURRENT NOVA REMNANT RS OPHIUCHI	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406033010/	Quick Look
326	V2487 OPH	262.9946	-19.3061	262.257209	-19.270365	263.364925	3.973676	6.53905762	7.73892052	274.1277	55478.2880439815	2010-10-09 06:54:47	55479.5827893518	2010-10-10 13:59:13	405021010	56.3076	50	56.3156	56.3076	0	56.3236	2	2	0	2	1	0	0	51.358	51.358	111.832	2	PROCESSED	57553.6771875	2016-06-14 16:15:09	55854	2011-10-20 00:00:00	55488.179224537	2010-10-19 04:18:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050059	Suzaku discovery of the first white dwarf pulsar, AE Aqr (Terada et.al 2008) had a great impact on the studies of the cosmic-ray origin, since white dwarfs were not recognized as a particle accelerator. The next step is to check whether this phenomenon is common or not. In order to search for the second white dwarf pulsar, we picked up hard objects among the INTEGRAL and Swift sample, and propose the Suzaku observation of the best two objects, V2487 Oph and IGRJ00234+6141.	GALACTIC POINT SOURCES	4	A	YUKIKATSU TERADA		JAP	5	AO5	SEARCH FOR NON-THERMAL EMISSION FROM HARD WHITE DWARFS WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405021010/	Quick Look
327	IGR J16207-5129	245.1895	-51.5038	244.232877	-51.38483	252.516177	-29.556104	332.45599844	-1.05021687	88.1855	54499.8231365741	2008-02-03 19:45:19	54500.7841898148	2008-02-04 18:49:14	402065010	0	0	0	0	0	0	0	0	0	0	1	0	0	49.5955	49.5955	83.0319	1	PROCESSED	57541.498587963	2016-06-02 11:57:58	54883	2009-02-21 00:00:00	54515.6347800926	2008-02-19 15:14:05	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/ver3.0/402065010/	Quick Look
328	SS 433	287.9531	4.9906	287.335307	4.906206	290.183209	27.182001	39.69950989	-2.2379409	78.6445	53829.6109606482	2006-04-04 14:39:47	53830.5327662037	2006-04-05 12:47:11	401003010	38.6767	40	38.6767	38.6767	38.6767	38.6767	2	2	2	2	1	0	0	28.2411	28.2411	79.634	1	PROCESSED	57533.395162037	2016-05-25 09:29:02	54394	2007-10-21 00:00:00	53906.1478125	2006-06-20 03:32:51	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010031	SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber.	GALACTIC POINT SOURCES	4	A	NOBUYUKI KAWAI		JAP	1	AO1	SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401003010/	Quick Look
329	HESS J1837-069	279.4395	-6.8651	278.765532	-6.909152	279.755327	16.256333	25.2664546	-0.10276403	102.6144	54164.5341898148	2007-03-05 12:49:14	54165.4286342593	2007-03-06 10:17:14	401026010	42.1911	40	42.1911	42.1991	0	42.2071	2	2	0	2	1	0	0	37.7021	37.7021	77.2599	1	PROCESSED	57537.6010185185	2016-05-29 14:25:28	54750	2008-10-11 00:00:00	54171.2613425926	2007-03-12 06:16:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010131	The HESS (High Energy Stereoscopic System) collaboration has recently reported the TeV survey of the inner-part of the Galaxy, which revealed the existence of a new population of gamma-ray objects. Most of which are unknown, but at least two of them, HESS J1813-178 and HESS J1837-069 are point-like, and the ASCA Galactic survey and the INTEGRAL survey detected the counterparts in 0.5-10 keV and 20-100 keV, respectively. Making full use of Suzaku's wide-band spectral capability, we will study spectral characteristics of HESS J1813-178 and HESS J1837-069 in 0.5 keV to ~200 keV, and investigate for their origins. We will also carry out pulse-search to evaluate the pulsar-wind hypothesis.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	1	AO1	INVESTIGATION OF TWO HESS SOURCES DETECTED WITH INTEGRAL	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401026010/	Quick Look
330	1RXS J070407.9+26250	106.0316	26.4199	105.25762	26.494968	104.352906	3.774212	190.26714041	14.29962915	96.1437	54749.1266319444	2008-10-10 03:02:21	54750.3682175926	2008-10-11 08:50:14	403003010	53.5519	50	53.5519	53.5519	0	53.5519	2	2	0	2	1	0	0	41.1405	41.1405	107.2319	0	PROCESSED	57544.1456944445	2016-06-05 03:29:48	55148	2009-11-13 00:00:00	54780.5445949074	2008-11-10 13:04:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030009	Soft Intermediate Polar (IP) is a group of IPs whose X-ray spectra are extremely soft compared with general IPs. Recent observations reveal that some soft IPs have a soft blackbody emission component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand comprehensively the emission characteristics of polars and IPs in the soft X-ray band, and to follow possible evolutionary link from IPs to polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure its temperature and flux systematically.	GALACTIC POINT SOURCES	4	B	MANABU ISHIDA		JAP	3	AO3	OBSERVATIONS OF SOFT INTERMEDIATE POLARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403003010/	Quick Look
331	1RX J154814.5-452845	237.0511	-45.4226	236.175049	-45.269354	245.126412	-24.783918	332.46961393	7.07040697	85.7358	54132.6368518518	2007-02-01 15:17:04	54135.3543865741	2007-02-04 08:30:19	401037010	99.4541	100	99.4541	99.4621	0	99.4701	2	2	0	2	1	0	0	86.8552	86.8552	234.7838	3	PROCESSED	57537.0252777778	2016-05-29 00:36:24	54702	2008-08-24 00:00:00	54139.4767939815	2007-02-08 11:26:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011102	Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber.	GALACTIC POINT SOURCES	4	A	KOJI MUKAI		USA	1	AO1	BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401037010/	Quick Look
332	WR140	305.1135	43.9272	304.692033	43.76792	327.425445	60.56194	80.98919394	4.21991141	90.2945	54565.231400463	2008-04-09 05:33:13	54565.7224305556	2008-04-09 17:20:18	403033010	21.6253	20	21.6253	21.6253	0	21.6253	2	2	0	2	1	0	0	18.6055	18.6055	42.4159	2	PROCESSED	57542.2656828704	2016-06-03 06:22:35	54953	2009-05-02 00:00:00	54580.4185648148	2008-04-24 10:02:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030157	WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	3	AO3	X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403033010/	Quick Look
333	4U 1705-44	257.2281	-44.1019	256.324944	-44.038193	260.193555	-21.093723	343.32141433	-2.34248879	264.0666	53996.5173611111	2006-09-18 12:25:00	53996.8619675926	2006-09-18 20:41:14	401046020	17.134	20	17.342	17.134	17.334	17.334	1	1	1	1	1	0	0	15.4477	15.4477	29.7679	0	PROCESSED	57535.6082175926	2016-05-27 14:35:50	54526	2008-03-01 00:00:00	54020.9055555556	2006-10-12 21:44:00	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011112	We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state.	GALACTIC POINT SOURCES	4	A	ANDREW YOUNG		USA	1	AO1	REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046020/	Quick Look
334	SWIFTJ2000.6+3210	300.0869	32.2033	299.597811	32.064769	312.685822	51.280995	68.99570836	1.1443147	87.4233	53837.6619212963	2006-04-12 15:53:10	53837.9139351852	2006-04-12 21:56:04	401053010	12.4384	20	12.444	12.4512	12.4512	12.4384	1	1	1	1	1	0	0	9.8767	9.8767	21.7679	0	PROCESSED	57533.4456134259	2016-05-25 10:41:41	54775	2008-11-05 00:00:00	53927.3549189815	2006-07-11 08:31:05	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011132	INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	1	AO1	HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401053010/	Quick Look
335	1RXSJ013106.4+612035	22.8032	61.3371	21.96963	61.079753	49.605162	46.981158	127.68400105	-1.16712133	215.0025	55993.5664930556	2012-03-07 13:35:45	55993.889837963	2012-03-07 21:21:22	406034020	12.1737	8	12.1737	12.1737	0	12.1737	2	2	0	2	1	0	0	17.897	17.897	27.9219	0	PROCESSED	57604.8011574074	2016-08-04 19:13:40	56374	2013-03-23 00:00:00	56008.1191782407	2012-03-22 02:51:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060097	We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray.	GALACTIC POINT SOURCES	4	B	HIROMITSU TAKAHASHI		JAP	6	AO6	SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406034020/	Quick Look
336	4U 0142+61	26.4803	61.7944	25.612931	61.544346	52.126454	46.446482	129.32255084	-0.39946076	40.959	54325.1695949074	2007-08-13 04:04:13	54327.5209259259	2007-08-15 12:30:08	402013010	99.6744	100	99.6744	99.6744	0	99.6744	2	2	0	2	1	0	0	101.6096	101.6096	203.1297	4	PROCESSED	57549.823900463	2016-06-10 19:46:25	54730	2008-09-21 00:00:00	54347.6221296296	2007-09-04 14:55:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020058	Recently, high energy pulsed x-ray emissions from anomalous x-ay pulsears have been founded. This emissions extend to neary 100 keV with photon index ~1, and the emission mechanism is unknown. In order to trace this enigmatic component, we propose the observation of the anomalous x-ray pulsar 4u 0142+61 with 100 ksec exposures. The main aim of this observation is to examine how high energy this emission extend to. Because the these emissions are almost 100% pulsed component, so using the pulse on-off method, we can achive the ultimate sensitivity not depending on the reproducibility of the background but depending only on the photon statistics. If the spectrum have the strong break neary ~250 keV, this emissions have originated as the compton scatterd photons in the star surface.	GALACTIC POINT SOURCES	4	A	TERUAKI ENOTO		JAP	2	AO2	THE PULSED HARD X-RAY EMISSION FROM ANOMALOUS X-RAY PULSAR 4U 0142+61	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402013010/	Quick Look
337	PSR B1259-63	195.6594	-63.8834	194.870087	-63.614735	227.713942	-50.940493	304.16424752	-1.0384525	292.9998	54330.0581481482	2007-08-18 01:23:44	54330.6877777778	2007-08-18 16:30:24	402014070	20.4812	20	20.4812	20.4812	0	20.4829	2	2	0	2	1	0	0	19.4703	19.4703	54.364	0	PROCESSED	57539.6	2016-05-31 14:24:00	54724	2008-09-15 00:00:00	54356.2228472222	2007-09-13 05:20:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014070/	Quick Look
338	SGR 0501+4516	75.2795	45.3414	74.367379	45.268539	78.857896	22.469212	161.49568149	1.98976538	93.3341	55060.8485069445	2009-08-17 20:21:51	55061.8348842593	2009-08-18 20:02:14	404078010	42.6753	40	42.6753	42.9553	0	42.8913	2	2	0	2	1	0	0	27.4878	27.4878	85.1858	0	PROCESSED	57548.1780092593	2016-06-09 04:16:20	54922	2009-04-01 00:00:00	55071.2594328704	2009-08-28 06:13:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	4	AO4	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404078010/	Quick Look
339	SS AUR	93.3423	47.7333	92.395757	47.74724	92.468681	24.321363	166.0127795	13.79596984	289.1089	54529.7508796296	2008-03-04 18:01:16	54530.180775463	2008-03-05 04:20:19	402045010	19.4714	20	19.4714	19.4714	0	19.4714	1	1	0	1	1	0	0	17.378	17.378	37.1359	0	PROCESSED	57541.7699074074	2016-06-02 18:28:40	54905	2009-03-15 00:00:00	54539.2223726852	2008-03-14 05:20:13	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/ver3.0/402045010/	Quick Look
340	4U1705-44	257.2244	-44.1021	256.321247	-44.038375	260.19074	-21.094172	343.31966899	-2.34047423	86.9924	54516.9847569444	2008-02-20 23:38:03	54517.6182175926	2008-02-21 14:50:14	402051030	25.9956	15	26.0516	25.9956	0	26.0516	2	2	0	2	1	0	0	20.8205	20.8205	54.7239	1	PROCESSED	57541.7148611111	2016-06-02 17:09:24	54901	2009-03-11 00:00:00	54535.2030439815	2008-03-10 04:52:23	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/ver3.0/402051030/	Quick Look
341	IGR J17544-2619	268.6038	-26.3314	267.825334	-26.322724	268.737527	-2.896537	3.23518966	-0.33446224	84.5765	54544.5263425926	2008-03-19 12:37:56	54547.2640509259	2008-03-22 06:20:14	402061010	103.4173	72	103.8115	103.8275	0	103.4173	2	2	0	2	1	0	0	65.5656	65.5656	236.5059	3	PROCESSED	57541.9752314815	2016-06-02 23:24:20	54933	2009-04-12 00:00:00	54566.6106134259	2008-04-10 14:39:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021121	Supergiant Fast X-ray Transients are a newly-discovered class of x-ray binary with short outbursts and late O to early B supergiant companions. They are not persistently bright, but the nature of their low-level variability is not well known. Similarly short outbursts are also seen in bright HMXBs with supergiant companions such as Cyg X-1 and Vel X-1. The mechanism of these outbursts is unknown in all cases. We propose long pointings to the two best-studied SFXTs and a third object, XTE J1743-363, which seems to be transitional between SFXTs and persistent supergiant HMXBs. We will characterize their variability at low flux levels, both to understand the accretion mechanism and to enable surveys of archival data for new SFXTs.	GALACTIC POINT SOURCES	4	C	DAVID SMITH		USA	2	AO2	CHARACTERIZING THE SPECTRUM AND VARIABILITY OF THE SUPERGIANT FAST X-RAY TRANSIENTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402061010/	Quick Look
342	EXO 2030+375	308.0118	37.6951	307.540549	37.524573	325.984128	54.001657	77.17399477	-1.17458429	56.3502	54234.8591666667	2007-05-14 20:37:12	54236.1565277778	2007-05-16 03:45:24	402068010	57.6071	40	57.6071	57.6071	0	57.6071	2	2	0	2	1	0	0	53.3954	53.3954	112.0678	2	PROCESSED	57538.7243055556	2016-05-30 17:23:00	54702	2008-08-24 00:00:00	54242.497962963	2007-05-22 11:57:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021124	We propose a 40 ks Suzaku observation to confirm EXO 2030+375's recently discovered ~10 keV cyclotron feature and constrain its second harmonic at ~20 keV. EXO 2030+375 is a 42-second Be/X-ray pulsar in an eccentric 46-day orbit. If confirmed the ~10 keV cyclotron feature will be the lowest in energy known for an accreting pulsar and will provide the missing piece to make EXO 2030+375 an ideal candidate to observationally test accretion theory. In addition, we will measure EXO 2030+375's spin frequency, study its pulse shape versus energy, and perform phase resolved spectroscopy. Suzaku will allow these studies to reach lower energies and provide high quality spectra at lower luminosities than in any previous observations.	GALACTIC POINT SOURCES	4	A	COLLEEN WILSON		USA	2	AO2	CONSTRAINING CYCLOTRON FEATURES IN A NORMAL OUTBURST OF EXO 2030+375	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402068010/	Quick Look
343	CYGNUS X-1	299.5814	35.2712	299.11183	35.134765	313.691248	54.317484	71.39067981	3.10930809	85.1433	54949.7099884259	2009-04-28 17:02:23	54950.2175925926	2009-04-29 05:13:20	404075050	20.5212	300	20.5292	20.5354	0	20.5212	2	1	0	2	1	0	0	12.4013	12.4013	43.8459	0	PROCESSED	57546.4475462963	2016-06-07 10:44:28	54922	2009-04-01 00:00:00	54976.2030671296	2009-05-25 04:52:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075050/	Quick Look
344	V2491 CYG	295.7679	32.3068	295.285617	32.186831	307.093304	52.481406	67.2208484	4.33923679	253.6206	55503.4390162037	2010-11-03 10:32:11	55505.2709837963	2010-11-05 06:30:13	405036010	74.4004	70	74.4004	74.4004	0	74.4004	2	2	0	2	1	0	0	57.2065	57.2065	158.2519	2	PROCESSED	57553.9866087963	2016-06-14 23:40:43	55885	2011-11-20 00:00:00	55518.4178356482	2010-11-18 10:01:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051213	We propose to observe again one of the most luminous and intriguing classical novae of the last two years, after it has returned to quiescence. The goala are to understand how accretion is re-estabilished, investigate the claim that the white dwarf an intermediate polar (IP), estimate mass accretion are and white dwarf mass. IP are a class of X-ray sources that Suzaku is ideally suited to study, and we want to study the influence of the magnetic field on the nova evolution.	GALACTIC POINT SOURCES	4	C	MARINA ORIO		USA	5	AO5	REVISITING AN X-RAY LUMINOUS NOVA NOVA AFTER THE ERUPTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405036010/	Quick Look
345	MARS-P10	103.2518	25.125	102.483772	25.186994	101.989505	2.233931	190.42954859	11.48582895	298.135	54560.0767708333	2008-04-04 01:50:33	54560.16	2008-04-04 03:50:24	403006100	3.7716	100	3.7956	3.7716	0	3.796	1	1	0	1	1	0	0	4.0014	4.0014	7.1839	0	PROCESSED	57542.0546527778	2016-06-03 01:18:42	54953	2009-05-02 00:00:00	54577.1537847222	2008-04-21 03:41:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006100/	Quick Look
346	GX 339-4	255.7297	-48.7352	254.782436	-48.66432	259.586148	-25.80756	338.99220289	-4.30584956	108.3513	54920.4773958333	2009-03-30 11:27:27	54921.5216435185	2009-03-31 12:31:10	403011030	39.6384	40	39.6633	39.6384	0	39.6633	2	2	0	2	1	0	0	35.0686	35.0686	90.186	0	PROCESSED	57545.9795601852	2016-06-06 23:30:34	55330	2010-05-14 00:00:00	54931.0610416667	2009-04-10 01:27:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030046	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	3	AO3-TOO	MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403011030/	Quick Look
347	MARS-P24	103.8389	25.0556	103.07157	25.120373	102.525763	2.214408	190.72046804	11.94011608	298.3401	54561.2433680556	2008-04-05 05:50:27	54561.3265509259	2008-04-05 07:50:14	403006240	3.423	100	3.423	3.423	0	3.423	1	1	0	1	1	0	0	2.511	2.511	7.1839	0	PROCESSED	57542.0844328704	2016-06-03 02:01:35	54953	2009-05-02 00:00:00	54578.1234375	2008-04-22 02:57:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006240/	Quick Look
348	TAU SCO	248.9714	-28.2185	248.191858	-28.116816	251.449018	-6.120961	351.53328031	12.80600635	277.9748	54710.0436689815	2008-09-01 01:02:53	54710.3697222222	2008-09-01 08:52:24	403034010	14.6171	10	14.6171	14.6171	0	14.6171	1	1	0	1	1	0	0	12.0855	12.0855	28.1359	0	PROCESSED	57543.4427777778	2016-06-04 10:37:36	55148	2009-11-13 00:00:00	54780.4170138889	2008-11-10 10:00:30	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/ver3.0/403034010/	Quick Look
349	GX 339-4	255.6944	-48.7333	254.747207	-48.662254	259.560211	-25.808209	338.97952784	-4.28620483	84.7264	54908.0786226852	2009-03-18 01:53:13	54908.9613310185	2009-03-18 23:04:19	403011010	43.0408	40	43.0554	43.0408	0	43.0614	1	1	0	1	1	0	0	35.3914	35.3914	76.2579	1	PROCESSED	57545.8736458333	2016-06-06 20:58:03	55330	2010-05-14 00:00:00	54917.4333796296	2009-03-27 10:24:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030046	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	3	AO3-TOO	MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403011010/	Quick Look
350	VW HYI	62.3036	-71.2936	62.394189	-71.422866	322.02345	-79.107148	284.88553906	-38.13260514	212.7427	55924.6383796296	2011-12-29 15:19:16	55925.1806828704	2011-12-30 04:20:11	406009020	16.1593	20	16.1593	16.1593	0	16.1593	2	2	0	2	1	0	0	13.7587	13.7587	46.8519	0	PROCESSED	57604.2667939815	2016-08-04 06:24:11	56313	2013-01-21 00:00:00	55945.9133912037	2012-01-19 21:55:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060023	SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate.	GALACTIC POINT SOURCES	4	B	KEI SAITOU		JAP	6	AO6-TOO	TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009020/	Quick Look
351	IGR J17303-0601	262.5864	-5.9814	261.916828	-5.94387	262.267561	17.260409	17.93788623	15.02149808	100.7922	54878.4233217593	2009-02-16 10:09:35	54879.3355787037	2009-02-17 08:03:14	403026010	32.9635	30	32.9635	32.9635	0	32.9635	2	2	0	2	1	0	0	27.7559	27.7559	78.818	2	PROCESSED	57545.5746990741	2016-06-06 13:47:34	55325	2010-05-09 00:00:00	54893.4381018518	2009-03-03 10:30:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030140	Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	3	AO3	IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403026010/	Quick Look
352	ETA CARINAE	161.3407	-59.6518	160.853368	-59.388342	202.155822	-58.871724	287.61551185	-0.58277566	142.0006	54856.1332291667	2009-01-25 03:11:51	54856.6821064815	2009-01-25 16:22:14	403037010	28.8053	30	28.8053	28.8053	0	28.8053	1	1	0	1	1	0	0	17.4539	17.4539	47.4079	0	PROCESSED	57545.3235185185	2016-06-06 07:45:52	55328	2010-05-12 00:00:00	54880.533587963	2009-02-18 12:48:22	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/ver3.0/403037010/	Quick Look
353	CEN X-4	224.5893	-31.6684	223.829289	-31.468804	231.309524	-14.121168	332.24097668	23.88258751	104.6233	54847.9102314815	2009-01-16 21:50:44	54850.9717939815	2009-01-19 23:19:23	403057010	146.6704	150	146.6876	146.6704	0	146.6916	2	2	0	2	1	0	0	133.6185	133.6185	264.4539	2	PROCESSED	57545.3354513889	2016-06-06 08:03:03	55328	2010-05-12 00:00:00	54880.5460069444	2009-02-18 13:06:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031161	Observations of thermal emission from the surface of quiescent neutron star low-mass X-ray binaries (LMXBs) can be used to measure neutron star radii. However, their quiescent spectra are complicated due to the presence of an additional power-law, and because variability has been seen on timescales as short as 100s. The nearest known neutron star LMXB Cen X-4 gives us the clearest view of these objects. But, the best observation so far lacked the sensitivity to determine the cause of the variability. Yet, the cause has important ramifications for measuring neutron star radii - if it is the thermal (rather than power-law) component that is varying our picture of quiescent emission may be wrong. To solve this critical problem we propose a 150 ksec observation of Cen X-4 with Suzaku.	GALACTIC POINT SOURCES	4	A	EDWARD CACKETT		USA	3	AO3	UNCOVERING VARIABLE QUIESCENT EMISSION IN THE NEUTRON STAR CEN X-4	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403057010/	Quick Look
354	AE AQUARII	310.0451	-0.9346	309.400522	-1.112531	312.21962	16.830556	45.22328928	-24.45613885	265.1622	55120.7618518518	2009-10-16 18:17:04	55124.2265393518	2009-10-20 05:26:13	404001010	160.4546	160	161.4519	161.7209	0	160.4546	2	2	0	2	1	0	0	136.0715	136.0715	299.3277	3	PROCESSED	57548.9948958333	2016-06-09 23:52:39	55503	2010-11-03 00:00:00	55134.5588194444	2009-10-30 13:24:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040032	As picked up in the NASA press release in 2008, one of the most important results with Suzaku in three years was the first discovery of a possible non-thermal pulsation from a white dwarf AE Aquarii. This job was performed by our group. "Can magnetized white dwarfs accelerate particles like neutron stars?" This is the basic question of this study as a long standing mystery of Cosmic-ray origin for near 100 years. To ensure our result with Suzaku, we triggered the guest observation of AE Aquarii in TeV gamma-ray band with the recent powerful telescope, H.E.S.S., in their first GO program on 2009. Here, we propose the simultaneous observation with Suzaku and H.E.S.S, to distinguish the acceleration site in and/or outer of the binary system using X-ray and TeV gamma-ray flux informations.	GALACTIC POINT SOURCES	4	A	YUKIKATSU TERADA		JAP	4	AO4	SUZAKU, H.E.S.S., OPTICAL SIMULTANEOUS OBSERVATION OF THE WHITE DWARF PULSAR, AE AQUARII	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404001010/	Quick Look
355	Z CAM	126.2993	73.0997	124.910098	73.261749	106.122719	51.687472	141.39550179	32.62975748	289.0998	54931.1187152778	2009-04-10 02:50:57	54931.9092476852	2009-04-10 21:49:19	404022010	37.663	35	37.663	37.663	0	37.663	2	2	0	2	1	0	0	36.5329	36.5329	68.2899	0	PROCESSED	57546.1159722222	2016-06-07 02:47:00	55324	2010-05-08 00:00:00	54949.4517824074	2009-04-28 10:50:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040095	The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail.	GALACTIC POINT SOURCES	4	B	KEI SAITOU		JAP	4	AO4	IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404022010/	Quick Look
356	AO PSC	343.7945	-3.1271	343.149274	-3.394015	343.859558	3.486369	68.69841137	-53.28578539	60.9461	55004.4934143518	2009-06-22 11:50:31	55005.3328587963	2009-06-23 07:59:19	404033010	39.6544	40	39.6544	39.6624	0	39.6624	2	2	0	2	1	0	0	35.6834	35.6834	72.5179	0	PROCESSED	57547.6306481482	2016-06-08 15:08:08	55385	2010-07-08 00:00:00	55018.165474537	2009-07-06 03:58:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040113	We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.	GALACTIC POINT SOURCES	4	A	TAKAYUKI YUASA		JAP	4	AO4	SURVEY OBSERVATION OF INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404033010/	Quick Look
357	4U 1608-52	243.2309	-52.3757	242.269732	-52.248184	251.350346	-30.651804	330.98178647	-0.83761569	125.7606	55273.9986689815	2010-03-18 23:58:05	55274.9154166667	2010-03-19 21:58:12	404044030	31.7568	30	31.7568	31.7568	0	31.7568	2	2	0	2	1	0	0	15.3094	15.3094	79.1938	0	PROCESSED	57550.9191898148	2016-06-11 22:03:38	55652	2011-04-01 00:00:00	55286.259849537	2010-03-31 06:14:11	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/ver3.0/404044030/	Quick Look
358	XTE J1710-281	257.5483	-28.1282	256.762614	-28.066297	258.983914	-5.161686	356.35839186	6.92613447	86.2275	55278.9207638889	2010-03-23 22:05:54	55281.1460300926	2010-03-26 03:30:17	404068010	76.1385	75	76.1385	76.1465	0	76.1465	3	3	0	3	1	0	0	23.6565	23.6565	192.2397	3	PROCESSED	57551.0466435185	2016-06-12 01:07:10	55668	2011-04-17 00:00:00	55301.5227662037	2010-04-15 12:32:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042003	We propose to observe XTE J1710-281, a low-mass X-ray binary showing bursts, eclipses and dips. We want to determine the nature of the X-ray emission in this yet poorly-studied system and exploit the fact it is viewed close to edge-on to probe the structure of the disk and of the ionized plasma located above it. The broad-band coverage of Suzaku XIS and HXD will allow us to determine the overall shape of the ionizing continuum, which is a key parameter to infer the properties of the warm absorber whose narrow spectral signatures will be simultaneously detected thanks to the good spectral resolution of XIS near 6 keV.	GALACTIC POINT SOURCES	4	C	LAURENCE BOIRIN		EUR	4	AO4	SUZAKU TO INVESTIGATE A LOW-MASS X-RAY BINARY SHOWING BURSTS, ECLIPSES, AND DIPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404068010/	Quick Look
359	BF ERI	69.8754	-4.5962	69.256008	-4.693413	67.473114	-26.478101	201.0367912	-31.29845078	262.0133	56350.9190625	2013-02-27 22:03:27	56351.6253009259	2013-02-28 15:00:26	407045010	32.8177	30	32.8177	32.8177	0	32.8178	3	3	0	3	1	0	0	32.0161	32.0161	61.0099	1	PROCESSED	57610.6930092593	2016-08-10 16:37:56	56738	2014-03-22 00:00:00	56372.5138773148	2013-03-21 12:19:59	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/ver3.0/407045010/	Quick Look
360	SCO X-1	245.0164	-15.3926	244.30666	-15.273445	245.822043	5.976116	359.32713596	23.91560488	98.4296	57090.7847685185	2015-03-09 18:50:04	57093.0903703704	2015-03-12 02:10:08	409025010	84.7086	50	0	0	0	84.7086	0	0	0	1	1	0	0	35.3772	35.3772	194.5699	0	PROCESSED	57617.8306365741	2016-08-17 19:56:07	57481	2016-04-03 00:00:00	57115.4052777778	2015-04-03 09:43:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090108	We propose 50 ks observation of the bright LMXB Sco X-1 (Z source) to search high energy emission above 50 keV and study Fe-K emission/absorption lines. With the combination of XIS and HXD, these properties can be studied with identifying the state of the source. Since Sco X-1 is so bright, the pointing is offset by ~15 arcmin from XIS nominal position.	GALACTIC POINT SOURCES	4	A	HIROMITSU TAKAHASHI		JAP	9	AO9	SUZAKU OBSERVATION OF THE BRIGHTEST LMXB SCO X-1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409025010/	Quick Look
361	CYGNUS X-1	299.6355	35.1397	299.165007	35.003038	313.68682	54.178773	71.30136328	3.00304649	241.2259	55152.2855092593	2009-11-17 06:51:08	55152.9418287037	2009-11-17 22:36:14	404075170	23.4485	300	23.4485	23.8885	0	23.8805	2	1	0	2	1	0	0	18.7071	18.7071	56.6918	3	PROCESSED	57549.4356597222	2016-06-10 10:27:21	54922	2009-04-01 00:00:00	55162.2019212963	2009-11-27 04:50:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075170/	Quick Look
362	CYGNUS X-1	299.6537	35.1518	299.183253	35.015061	313.717721	54.185168	71.31947353	2.99665901	225.8159	55166.2922453704	2009-12-01 07:00:50	55166.8904398148	2009-12-01 21:22:14	404075190	22.4155	300	22.4155	22.4315	0	22.4235	2	1	0	2	1	0	0	13.1578	13.1578	51.6739	0	PROCESSED	57549.6647222222	2016-06-10 15:57:12	54922	2009-04-01 00:00:00	55181.288912037	2009-12-16 06:56:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075190/	Quick Look
363	J1803-2149	270.7914	-21.8184	270.03917	-21.820419	270.725404	1.620434	8.14241987	0.18738401	269.7005	56191.3371643518	2012-09-21 08:05:31	56192.1730671296	2012-09-22 04:09:13	407092010	31.9986	25	32.0218	32.0146	0	31.9986	2	2	0	2	1	0	0	28.8812	28.8812	72.2179	1	PROCESSED	57607.1276736111	2016-08-07 03:03:51	56584	2013-10-19 00:00:00	56218.5534259259	2012-10-18 13:16:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072019	The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances.	GALACTIC POINT SOURCES	4	A	MARTINO MARELLI		EUR	7	AO7	SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407092010/	Quick Look
364	SAGITTARIUS A*	266.4154	-29.0072	265.620691	-28.987862	266.840925	-5.605376	359.94411521	-0.04477398	105.699	56752.451400463	2014-04-05 10:50:01	56752.9848611111	2014-04-05 23:38:12	408017090	22.1668	20	22.1668	23.5591	0	23.5701	2	2	0	2	1	0	0	18.8745	18.8745	46.0878	1	PROCESSED	57614.1690740741	2016-08-14 04:03:28	57134	2015-04-22 00:00:00	56768.7215856482	2014-04-21 17:19:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017090/	Quick Look
365	PSR J2055+2539	313.957	25.6505	313.412506	25.458222	325.920666	40.944888	70.67687842	-12.53222207	262.3229	55498.1479398148	2010-10-29 03:33:02	55498.9578356482	2010-10-29 22:59:17	405015010	31.1069	30	31.1069	31.1069	0	31.1069	1	1	0	1	1	0	0	21.4581	21.4581	69.9679	0	PROCESSED	57553.8967592593	2016-06-14 21:31:20	55890	2011-11-25 00:00:00	55523.9927314815	2010-11-23 23:49:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050047	Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.	GALACTIC POINT SOURCES	4	C	NOBUYUKI KAWAI		JAP	5	AO5	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405015010/	Quick Look
366	4U 1957+11	299.8418	11.7197	299.250981	11.582408	304.890304	31.617141	51.31351001	-9.31745051	63.9325	55333.5190277778	2010-05-17 12:27:24	55334.4675	2010-05-18 11:13:12	405057020	34.9353	35	34.9433	34.9513	0	34.9353	2	2	0	2	1	0	0	28.2625	28.2625	81.9118	0	PROCESSED	57551.562650463	2016-06-12 13:30:13	55714	2011-06-02 00:00:00	55347.2466898148	2010-05-31 05:55:14	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/ver3.0/405057020/	Quick Look
367	SWIFT J1834.9-0846	278.7285	-8.7724	278.045132	-8.813015	278.89774	14.398942	23.24882887	-0.35409613	264.9986	56582.3041319444	2013-10-17 07:17:57	56583.3335300926	2013-10-18 08:00:17	408015010	35.9317	40	38.1117	38.1117	0	35.9317	2	2	0	3	1	0	0	31.9264	31.9264	88.9319	1	PROCESSED	57613.0148726852	2016-08-13 00:21:25	56967	2014-11-06 00:00:00	56601.6309953704	2013-11-05 15:08:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080040	Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources.	GALACTIC POINT SOURCES	4	B	TERUAKI ENOTO		JAP	8	AO8	ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408015010/	Quick Look
368	GX 339-4	255.7041	-48.783	254.756356	-48.711998	259.573299	-25.856913	338.94384752	-4.32149031	92.8952	55627.5468518518	2011-03-07 13:07:28	55628.0320138889	2011-03-08 00:46:06	405063050	16.9925	20	16.9925	20.2693	0	20.2693	2	2	0	2	1	0	0	15.9851	15.9851	41.8741	2	PROCESSED	57601.1142476852	2016-08-01 02:44:31	56015	2012-03-29 00:00:00	55645.2088078704	2011-03-25 05:00:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052015	We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4	GALACTIC POINT SOURCES	4	A	CLEMENT CABANAC		EUR	5	AO5-TOO	PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063050/	Quick Look
369	PSR J0726-2612	111.531	-26.2114	111.017873	-26.110384	119.169713	-47.49417	240.07877209	-4.64696128	117.9984	55881.5691782407	2011-11-16 13:39:37	55882.6252546296	2011-11-17 15:00:22	406012010	43.757	100	43.757	43.792	0	43.792	2	2	0	2	1	0	0	39.7288	39.7288	91.2278	0	PROCESSED	57603.8172685185	2016-08-03 19:36:52	56264	2012-12-03 00:00:00	55895.2388078704	2011-11-30 05:43:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060041	To study the origin of magnetars, a unique opportunity is provided by detecting an excess of thermal radiation in the radio pulsars which has dipolar magnetic fields as high as magnetars. The excess is caused by field decay as seen in magnetars. A question is raised whether the rotation powered pulsars can have active magnetic flux similar to magnetars. PSR J0726-2612 is a nearby (3kpc) radio pulsar with magnetic field as high as 10^13.5 G, and therefore is an ideal target. We propose 100ksec observation of this pulsar to discover magnetar-like thermal radiation, and determine the structure of the active magnetic flux tubes by phase alignment of rotational modulation of the X-ray radiation with radio pulses.	GALACTIC POINT SOURCES	4	C	SHINPEI SHIBATA		JAP	6	AO6	CAN HIGH MAGNETIC FIELD RADIO PULSARS BE THE MAGNETAR ?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406012010/	Quick Look
370	SGR 1806-20	272.1607	-20.4008	271.416415	-20.409492	272.01832	3.024829	10.00344249	-0.23433657	89.0334	56010.449837963	2012-03-24 10:47:46	56012.5314814815	2012-03-26 12:45:20	406069010	70.5964	70	70.5964	70.5964	0	70.5964	2	2	0	2	1	0	0	63.9571	63.9571	179.8279	2	PROCESSED	57605.0500462963	2016-08-05 01:12:04	56399	2013-04-17 00:00:00	56023.2387384259	2012-04-06 05:43:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061301	Recent Suzaku investigations revealed that a broad-band (0.8-70 keV) spectra of known magnetars systematically change depending on their characteristic ages. The hard X-rays of magnetars become weaker but harder for older objects. In order to accomplish this picture, we have to verify that this correlation is rather free from selection effects, and holds even when the sources vary on long time scales. Here we propose a 70 ks observation of SGR 1806-20. If we detect the hard X-rays from this source at a rather intensity, the above correlation will be much reinforced.	GALACTIC POINT SOURCES	4	C	TERUAKI ENOTO		USA	6	AO6	VARIABILITY OF HARD X-RAYS FROM MAGNETARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406069010/	Quick Look
371	AX J1818.8-1559	274.7184	-16.0002	273.997976	-16.021361	274.56335	7.365738	15.02984997	-0.2600064	265.8517	55849.5538888889	2011-10-15 13:17:36	55852.1474537037	2011-10-18 03:32:20	406074010	95.1912	100	99.3859	99.3859	0	95.1912	2	2	0	2	1	0	0	83.8746	83.8746	224.0699	1	PROCESSED	57603.4900347222	2016-08-03 11:45:39	56241	2012-11-10 00:00:00	55873.993599537	2011-11-08 23:50:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062016	The Galactic X-ray source AX J1818.8-1559 is a possible new member of the small class of magnetar candidates since a short and soft burst was detected in the 15--100 keV range from this source in 2007 with INTEGRAL. We request a Suzaku pointing of 100 ks in order to carry out a sensitive search for pulsations. This, together with the good quality spectrum, possibly extending in the hard X-ray range, that can be obtained with the Suzaku instruments, will allow us to reveal the nature of AX J1818.8-1559, most likely adding a new member to the small but rapidly increasing family of magnetar candidates	GALACTIC POINT SOURCES	4	B	SANDRO MEREGHETTI		EUR	6	AO6	A NEW GALACTIC MAGNETAR CANDIDATE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406074010/	Quick Look
372	MRK 520	330.1768	10.545	329.561779	10.304216	336.215385	21.249415	69.38972894	-34.038497	250.5002	56258.8186458333	2012-11-27 19:38:51	56260.6571412037	2012-11-29 15:46:17	407014010	79.7795	80	79.7795	79.7875	0	79.7955	2	2	0	2	1	0	0	77.641	77.641	158.8258	1	PROCESSED	57608.1523263889	2016-08-08 03:39:21	56644	2013-12-18 00:00:00	56275.7255555556	2012-12-14 17:24:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070028	Compton-thick AGNs contribute to the hard X-ray background and are key objects for investigating the cosmological evolution of AGNs. But heavy obscuration under 10 keV, and source misidentification mean that very few sources have been studied in detail. We have developed new infrared and hard X-ray diagnostics of AGN identification, based on which we select one candidate, Mrk 520, which must be very highly obscured and likely Compton-thick. With Suzaku, we will characterize all emission components, not only thermal and scattering components under 10 keV, but also the heavily obscured continuum over 10 keV, and reflection components.	GALACTIC POINT SOURCES	4	C	KEIKO MATSUTA		JAP	7	AO7	MRK 520 : A NEW COMPTON-THICK AGN?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407014010/	Quick Look
373	IGR J17091-3624	257.2807	-36.4071	256.440218	-36.343795	259.493682	-13.428104	349.52434208	2.21333885	90.7245	56342.7065162037	2013-02-19 16:57:23	56344.8856828704	2013-02-21 21:15:23	407037020	81.9467	80	81.9467	81.9467	0	81.9467	2	2	0	2	1	0	0	72.871	72.871	188.26	1	PROCESSED	57610.6944212963	2016-08-10 16:39:58	56728	2014-03-12 00:00:00	56363.6146990741	2013-03-12 14:45:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070097	We propose a Suzaku observation of "the second GRS 1915+105" IGR J17091-3624 with a high energy resolution and broadband capability. GRS 1915+105 has been considered to be the unique black hole binary that stays at a high mass accretion rate and shows limit-cycle oscillations, but it was recently discovered that the BHC IGR J17091-3624 has exactly the same X-ray variability patterns as GRS 1915+105. This fact suggests an evidence for common physical mechanism in both system. The Suzaku observation will reveal both similarity and difference with GRS 1915+105 from a point of view of broad-band spectral properties and disk wind, and help us understanding of the accretion flow onto a black hole under a high mass accretion rate.	GALACTIC POINT SOURCES	4	B	KAZUTAKA YAMAOKA		JAP	7	AO7	SUZAKU BROADBAND OBSERVATION OF "THE SECOND GRS 1915+105" IGR J17091-3624	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407037020/	Quick Look
374	X 1630-472	248.5014	-47.3935	247.58039	-47.289358	254.085874	-25.131659	336.90846442	0.25253242	88.6317	57073.2374884259	2015-02-20 05:41:59	57074.4111805556	2015-02-21 09:52:06	409007010	6.1528	40	6.165	6.1823	0	6.1528	3	3	0	3	0	0	0	0	0	0	0	PROCESSED	57617.6570023148	2016-08-17 15:46:05	57454	2016-03-07 00:00:00	57087.4573032407	2015-03-06 10:58:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090015	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	9	AO9-TOO	MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409007010/	Quick Look
375	1FGL J1018.6-5856	154.7397	-58.9449	154.297065	-58.693515	196.565416	-60.867795	284.35462729	-1.68677577	302.8974	56098.9298611111	2012-06-20 22:19:00	56100.4612384259	2012-06-22 11:04:11	407069010	72.8412	70	72.8412	72.8412	0	72.8412	2	2	0	2	1	0	0	57.6773	57.6773	132.25	0	PROCESSED	57605.7791087963	2016-08-05 18:41:55	56479	2013-07-06 00:00:00	56113.258900463	2012-07-05 06:12:49	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/ver3.0/407069010/	Quick Look
376	J1746-3239	266.7261	-32.6662	265.90725	-32.648308	267.198391	-9.25684	356.95543166	-2.17351712	72.0153	56365.6469675926	2013-03-14 15:31:38	56366.4022453704	2013-03-15 09:39:14	407093010	27.3469	25	27.3469	27.3469	0	27.3469	2	2	0	2	1	0	0	27.005	27.005	65.2519	2	PROCESSED	57610.8216087963	2016-08-10 19:43:07	56745	2014-03-29 00:00:00	56379.530775463	2013-03-28 12:44:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072019	The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances.	GALACTIC POINT SOURCES	4	A	MARTINO MARELLI		EUR	7	AO7	SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407093010/	Quick Look
377	4U 0614+091	94.2788	9.1363	93.59351	9.155405	94.360649	-14.24001	200.87717258	-3.36522944	89.7995	56579.4227314815	2013-10-14 10:08:44	56580.8314351852	2013-10-15 19:57:16	408009010	33.687	60	33.687	34.6474	0	34.9366	3	4	0	4	1	0	0	57.7016	57.7016	121.6639	0	PROCESSED	57612.9715393518	2016-08-12 23:19:01	57144	2015-05-02 00:00:00	56601.6144791667	2013-11-05 14:44:51	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080028	We propose an Suzaku observation of LMXB 4U 0614+091 for the study of Neutron Star Binary (NSB) in the low/hard state. An aim of this observation is to reveal a physical model of the NSB low/hard state in a same analogy of Black-Hole Binary (BHB) low/hard state. In the BHB Cyg X-1, the spectra in low/hard state radiate from a cool accretion disk and a hot comptonizing corona. A spectra of NS in low/hard state would have the same structure as Cyg X-1, but it is hard to study the fine structure of the spectra because of low luminosity. Suzaku can determine the low temperature of the disk and the high temperature of the corona, thanks to wide-band and high sensitivity detectors: XIS/BI and HXD. This observation is important for an unified model between BHB and NSB.	GALACTIC POINT SOURCES	4	B	SATOSHI SUGITA		JAP	8	AO8	THE SPECTRAL STUDY OF LMXB 4U 0614+091 IN THE LOW/HARD STATE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408009010/	Quick Look
378	SAGITTARIUS A*	266.415	-29.006	265.620299	-28.98666	266.840543	-5.604185	359.94495727	-0.04385023	107.0004	56744.9007523148	2014-03-28 21:37:05	56745.6238541667	2014-03-29 14:58:21	408017080	20.4818	20	20.4917	20.5036	0	20.4818	3	3	0	3	1	0	0	19.7498	19.7498	62.4719	1	PROCESSED	57614.1384837963	2016-08-14 03:19:25	57121	2015-04-09 00:00:00	56756.7635185185	2014-04-09 18:19:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017080/	Quick Look
379	V1223 SGR	283.7576	-31.1629	282.952803	-31.227217	281.857553	-8.28711	4.95796111	-14.35306818	89.5992	56757.9023611111	2014-04-10 21:39:24	56761.5211111111	2014-04-14 12:30:24	408019020	150.7683	60	150.7763	150.7763	0	150.7683	2	2	0	2	1	0	0	146.3158	146.3158	312.6057	3	PROCESSED	57614.3279976852	2016-08-14 07:52:19	57152	2015-05-10 00:00:00	56789.7985648148	2014-05-12 19:09:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080086	A 180-ks observation of the magnetic cataclysmic variable V1223 Sgr is proposed. By increasing the statistics by a factor of 4 compared to the existing 45-ks data, we investigate spin-phase dependent redshift of the iron fluorescent line, in particular its line center energy and equivalent width with smaller statistical errors than results of Hayashi et al. 2011. These parameters will provide geometrical configuration, or solid angle viewed from the post-shock region, of the pre-shock cool gas and the white dwarf reflecting surface. We use this information to make our Monte-Carlo simulator of magnetic CV more physically realistic and reliable in analyzing the high-resolution iron line profiles to be obtained with the ASTRO-H/SXS.	GALACTIC POINT SOURCES	4	B	TAKAYUKI YUASA		JAP	8	AO8	DEEP OBSERVATION OF THE MAGNETIC CATACLYSMIC VARIABLE V1223 SGR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408019020/	Quick Look
380	GX 339-4	255.7085	-48.7866	254.760711	-48.715619	259.576938	-25.860175	338.94274721	-4.32598042	275.4008	56526.5726967593	2013-08-22 13:44:41	56529.3592476852	2013-08-25 08:37:19	408034010	101.0196	100	101.0196	101.0196	0	101.0196	2	2	0	2	1	0	0	90.3169	90.3169	240.7097	1	PROCESSED	57612.5083680556	2016-08-12 12:12:03	56956	2014-10-26 00:00:00	56588.9590046296	2013-10-23 23:00:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081242	Due to the presence of a steady jet, constraining the properties of black hole systems in their hard state is important for understanding accretion disks and jets. 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? This proposal includes the use of Suzaku, NuSTAR, and radio observations to address these questions. A main diagnostic of the accretion geometry is the Compton reflection component, and the combination of Suzaku and NuSTAR covers, with very good energy resolution and sensitivity, the iron emission line, the absorption edges, and the hard X-ray reflection bump.	GALACTIC POINT SOURCES	4	A	JOHN TOMSICK		USA	8	AO8-TOO	CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408034010/	Quick Look
381	SAGITTARIUS A*	266.415	-29.0097	265.620276	-28.99036	266.840636	-5.607884	359.94179901	-0.04577777	105.7704	57095.3193171296	2015-03-14 07:39:49	57096.4952777778	2015-03-15 11:53:12	409011030	25.5496	20	25.5496	47.3551	0	47.3522	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.7910763889	2016-08-17 18:59:09	56748	2014-04-01 00:00:00	57111.394525463	2015-03-30 09:28:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090048	With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	9	AO9	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011030/	Quick Look
382	1RXS J032540.0-08144	51.413	-8.2453	50.804131	-8.420115	46.598209	-26.061844	192.86854593	-48.95490782	66.7974	56869.0655208333	2014-07-31 01:34:21	56869.9960532407	2014-07-31 23:54:19	409029010	39.5408	40	39.5408	39.9168	0	39.9248	2	2	0	2	1	0	0	18.9289	18.9289	53.612	0	PROCESSED	57616.4538425926	2016-08-16 10:53:32	57264	2015-08-30 00:00:00	56898.3797453704	2014-08-29 09:06:50	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/ver3.0/409029010/	Quick Look
383	CYGNUS X-1	299.5796	35.2119	299.109658	35.075474	313.654707	54.262131	71.33922039	3.07967202	58.5817	56796.2767476852	2014-05-19 06:38:31	56799.3266203704	2014-05-22 07:50:20	409049010	14.5127	30	0	14.5127	0	0	0	3	0	0	1	0	0	113.8259	113.8259	263.4619	1	PROCESSED	57615.2053703704	2016-08-15 04:55:44	57180	2015-06-07 00:00:00	56811.8023958333	2014-06-03 19:15:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091241	We propose for a 30 ks observation of the accreting black hole Cygnus X-1 to occur simultaneously with NuSTAR. In mid-2012, we obtained a joint Suzaku/NuSTAR observation of Cyg X-1 in the soft state, and we clearly see reflection features with a relativistically broadened iron line that we have used to constrain the geometry of the accretion disk, including finding possible evidence for a warped accretion disk, and the black hole spin. This TOO proposal is to observe the source in the hard state to constrain how the accretion geometry changes between states. The combination of Suzaku and NuSTAR covers, with very good energy resolution and throughput, the thermal component, the iron line complex, the iron absorption edge, and the hard X-ray reflection hump.	GALACTIC POINT SOURCES	4	A	JOHN TOMSICK		USA	9	AO9-TOO	CYGNUS X-1 IN THE HARD STATE WITH SUZAKU AND NUSTAR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409049010/	Quick Look
384	X1630-472	248.5239	-47.3401	247.603368	-47.236061	254.092996	-25.076506	336.95804041	0.27755382	107.6616	53809.226412037	2006-03-15 05:26:02	53809.743912037	2006-03-15 17:51:14	400010050	23.1671	200	23.1751	23.1769	23.1768	23.1671	2	1	2	2	1	0	0	18.8605	18.8605	44.706	0	PROCESSED	57533.2189930556	2016-05-25 05:15:21	54247	2007-05-27 00:00:00	54041.9302662037	2006-11-02 22:19:35	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/ver3.0/400010050/	Quick Look
385	CH CYG	291.1168	50.2494	290.78804	50.14985	313.638835	70.5089	81.85997028	15.59541424	38.1861	53883.3112962963	2006-05-28 07:28:16	53884.1502199074	2006-05-29 03:36:19	400016030	35.144	35	35.152	35.16	35.16	35.144	1	1	1	1	1	0	0	37.459	37.459	72.4479	1	PROCESSED	57534.4573726852	2016-05-26 10:58:37	54258	2007-06-07 00:00:00	54109.7043981482	2007-01-09 16:54:20	3.0.22.43	9	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/ver3.0/400016030/	Quick Look
386	SGR1900+14	286.803	9.3875	286.206177	9.3084	289.573902	31.693472	43.07594962	0.80149907	86.5533	53826.3631597222	2006-04-01 08:42:57	53826.9113310185	2006-04-01 21:52:19	401022010	17.0562	20	17.7046	21.7074	21.6555	17.0562	1	2	1	1	1	0	0	14.3604	14.3604	47.336	1	PROCESSED	57533.34875	2016-05-25 08:22:12	54394	2007-10-21 00:00:00	53906.0977893518	2006-06-20 02:20:49	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010124	We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs.	GALACTIC POINT SOURCES	4	A	YUJIN NAKAGAWA		JAP	1	AO1-TOO	PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR"	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401022010/	Quick Look
387	CYGNUS X-2	326.1653	38.3323	325.647427	38.10178	346.69525	47.972917	87.3318132	-11.3049847	76.3142	53871.8636805556	2006-05-16 20:43:42	53872.7293171296	2006-05-17 17:30:13	401049010	39.3903	37	39.3903	39.4063	39.3903	39.3903	2	1	2	2	1	0	0	36.8804	36.8804	74.786	1	PROCESSED	57534.3858217593	2016-05-26 09:15:35	54401	2007-10-28 00:00:00	53927.6429166667	2006-07-11 15:25:48	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011113	The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme.	GALACTIC POINT SOURCES	4	B	JON MILLER		USA	1	AO1	A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401049010/	Quick Look
388	1E 1841-045	280.3141	-4.8735	279.649841	-4.921767	280.812771	18.180712	27.4352849	0.03686802	77.3227	53844.4525462963	2006-04-19 10:51:40	53847.1328009259	2006-04-22 03:11:14	401100010	97.9622	100	97.9622	97.9702	97.9709	97.9709	2	2	2	2	1	0	0	63.474	63.474	231.5399	2	PROCESSED	57533.5748032407	2016-05-25 13:47:43	54401	2007-10-28 00:00:00	53907.2806597222	2006-06-21 06:44:09	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014204	Anomalous X-ray Pulsars are young radio-quiet pulsars with unconventional properties challenging conventional wisdom on neutron star formation and evolution. Their slow rotation periods, unprecedented for their apparent youth, point to enormous surface magnetic fields, a thousand times stronger than the typical inferred radio-pulsar field. The origin of the X-ray emission from these pulsars is still being debated. The recent discovery of a hard nonthermal pulsed X-ray emission from 1E 1841-045 with RXTE well beyond 10keV, can probably be explain by a magnetospheric origin and should extend above 100keV. The HXD onboard Suzaku gives us a unique opportunity to characterize the high-energy part of the emission with the added advantage to use the XIS to characterize the lower energy data.	GALACTIC POINT SOURCES	4	A	ILANA HARRUS	MIKIO NORII	USJ	1	AO1	SUZAKU OBSERVATIONS OF THE ANOMALOUS X-RAY PULSAR 1E~1841-045 IN THE SNR KES 73	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401100010/	Quick Look
389	SIGMA GEM	115.843	28.9438	115.063071	29.063433	112.630716	7.510513	191.13214337	23.30670736	104.4403	54394.4090162037	2007-10-21 09:48:59	54397.9690162037	2007-10-24 23:15:23	402033010	142.8897	125	142.8897	142.9936	0	142.9856	2	2	0	2	1	0	0	124.4471	124.4471	307.5416	1	PROCESSED	57540.4020138889	2016-06-01 09:38:54	54776	2008-11-06 00:00:00	54407.830474537	2007-11-03 19:55:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021014	Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission on RS CVn binaries. We propose a 125 ksec (3-4 day elapsed time) observation of the RS CVn binary Sigma Gem. Our goals are i) to better characterize its hard (>10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data, and iv) compare long duration flares on Sigma Gem with the 6 hour flares of Sigma2 CrB. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability at 10-25 keV provided by HXD.	GALACTIC POINT SOURCES	4	C	ALEXANDER BROWN		USA	2	AO2	SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL STRUCTURE ON THE RS CVN BINARY SIGMA GEM (K0III +?)	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402033010/	Quick Look
390	AQL X-1	287.8181	0.5776	287.17982	0.493878	289.379	22.827401	35.7124509	-4.14763067	265.5384	54392.3838310185	2007-10-19 09:12:43	54392.7918287037	2007-10-19 19:00:14	402053050	17.8899	15	17.8899	17.8899	0	17.8899	1	1	0	1	1	0	0	16.9278	16.9278	35.2319	1	PROCESSED	57540.3079513889	2016-06-01 07:23:27	54769	2008-10-30 00:00:00	54402.4178935185	2007-10-29 10:01:46	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/ver3.0/402053050/	Quick Look
391	TW HYA	165.4619	-34.7081	164.870404	-34.438931	182.672236	-37.188941	278.67685486	22.95004903	99.3673	54429.0615625	2007-11-25 01:28:39	54429.6946064815	2007-11-25 16:40:14	402089020	20.0096	11	20.0096	20.0176	0	20.0256	1	1	0	1	1	0	0	17.55	17.55	54.6879	2	PROCESSED	57540.5900115741	2016-06-01 14:09:37	54804	2008-12-04 00:00:00	54434.1387268518	2007-11-30 03:19:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022007	We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra.	GALACTIC POINT SOURCES	4	B	JURGEN SCHMITT		EUR	2	AO2	ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402089020/	Quick Look
392	4 DRA	187.4841	69.1938	186.936079	69.469913	136.91907	61.165888	125.77229084	47.81569563	339.9969	55304.8913773148	2010-04-18 21:23:35	55305.8557291667	2010-04-19 20:32:15	405035010	42.2602	40	42.2682	42.2682	0	42.2602	2	2	0	2	1	0	0	43.792	43.792	83.2778	1	PROCESSED	57551.2555439815	2016-06-12 06:07:59	55693	2011-05-12 00:00:00	55327.2173958333	2010-05-11 05:13:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051212	The symbiotic star, 4 Dra, has been poorly studied in X-rays. Based on the ROSAT data, we argue that it is a nearby, lower accretion rate analogue of the hard X-ray bright symibiotic stars that have been detected above 10 keV. We propose the first pointed observation of 4 Dra that covers the entire 0.4-10 keV band to test our interpretation: we expect it to be bright above 2 keV, with an optically thin thermal spectrum, likely with a strong and complex intrinsic absorber. If confirmed, 4 Dra may turn out to be a key object in the study of hard X-ray emitting symbiotic stars.	GALACTIC POINT SOURCES	4	B	KOJI MUKAI		USA	5	AO5	THE FIRST LOOK AT THE SYMBIOTIC STAR 4 DRA ABOVE 2 KEV	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405035010/	Quick Look
393	MARS-P2	102.9198	25.1641	102.151384	25.224519	101.686434	2.245784	190.26475308	11.2294146	298.0203	54559.4100925926	2008-04-03 09:50:32	54559.493275463	2008-04-03 11:50:19	403006020	4.8546	100	4.8546	4.8866	0	4.8706	1	1	0	1	1	0	0	3.6121	3.6121	7.1839	0	PROCESSED	57542.0367939815	2016-06-03 00:52:59	54953	2009-05-02 00:00:00	54577.0304976852	2008-04-21 00:43:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006020/	Quick Look
394	MARS-P19	103.6272	25.0809	102.859615	25.144671	102.332327	2.221472	190.61541806	11.77628093	298.2673	54560.8266319444	2008-04-04 19:50:21	54560.9098842593	2008-04-04 21:50:14	403006190	2.8398	100	2.8398	2.8482	0	2.8438	2	2	0	2	1	0	0	1.8441	1.8441	7.19	0	PROCESSED	57542.0723958333	2016-06-03 01:44:15	54953	2009-05-02 00:00:00	54578.0465625	2008-04-22 01:07:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006190/	Quick Look
395	1A1118-61	170.3073	-61.878	169.75636	-61.603723	210.888825	-57.212599	292.515895	-0.84430143	131.7127	54846.5144328704	2009-01-15 12:20:47	54847.9029976852	2009-01-16 21:40:19	403049010	49.6674	45	49.6674	49.6674	0	49.6674	2	2	0	2	1	0	0	46.8159	46.8159	119.9538	0	PROCESSED	57545.2346296296	2016-06-06 05:37:52	55328	2010-05-12 00:00:00	54858.6603125	2009-01-27 15:50:51	3.0.22.43	5	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/ver3.0/403049010/	Quick Look
396	IGR J17195-4100	259.8947	-41.0152	259.016072	-40.964234	261.995287	-17.853831	346.97641748	-2.13400756	97.0631	54880.4607175926	2009-02-18 11:03:26	54881.3106481482	2009-02-19 07:27:20	403028010	31.6456	30	31.6456	31.6456	0	31.6456	2	2	0	2	1	0	0	26.9178	26.9178	73.428	0	PROCESSED	57545.5868981482	2016-06-06 14:05:08	55330	2010-05-14 00:00:00	54895.5494328704	2009-03-05 13:11:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030140	Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	3	AO3	IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403028010/	Quick Look
397	ETA CARINAE	161.2769	-59.635	160.789962	-59.371642	202.089433	-58.883736	287.57915278	-0.58292483	99.9027	54810.21125	2008-12-10 05:04:12	54811.2084953704	2008-12-11 05:00:14	403036010	48.5016	30	48.5016	48.5016	0	48.5016	2	2	0	2	1	0	0	42.4259	42.4259	86.1518	2	PROCESSED	57544.6853125	2016-06-05 16:26:51	55198	2010-01-02 00:00:00	54828.3640972222	2008-12-28 08:44:18	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/ver3.0/403036010/	Quick Look
398	4U 1820-30	275.9316	-30.4206	275.12802	-30.447431	275.142418	-7.085697	2.73970623	-7.95024046	261.8755	55096.0447453704	2009-09-22 01:04:26	55096.8335416667	2009-09-22 20:00:18	404069030	29.2254	20	29.2254	29.2254	0	29.2254	2	1	0	2	1	0	0	25.9405	25.9405	68.148	1	PROCESSED	57548.6598726852	2016-06-09 15:50:13	55477	2010-10-08 00:00:00	55110.3989699074	2009-10-06 09:34:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069030/	Quick Look
399	CYGNUS X-1	299.6086	35.1319	299.138103	34.995352	313.646938	54.178814	71.28321336	3.01775246	259.2069	55130.2652314815	2009-10-26 06:21:56	55130.7481365741	2009-10-26 17:57:19	404075140	23.1042	300	23.1042	23.1282	0	23.1202	2	1	0	2	1	0	0	20.011	20.011	41.716	0	PROCESSED	57548.9943171296	2016-06-09 23:51:49	54922	2009-04-01 00:00:00	55141.3539467593	2009-11-06 08:29:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075140/	Quick Look
400	RXJ2056.6+4940	314.1926	49.6559	313.786825	49.462572	344.783467	62.123143	89.31769097	2.74712249	241.0011	55887.7886805556	2011-11-22 18:55:42	55888.5355208333	2011-11-23 12:51:09	406014010	42.3731	40	42.3811	42.3731	0	42.3731	2	2	0	2	1	0	0	44.6665	44.6665	64.524	1	PROCESSED	57603.9503356482	2016-08-03 22:48:29	56264	2012-12-03 00:00:00	55897.0994791667	2011-12-02 02:23:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060065	There are a total 1451 gamma-ray emitting objects in the Fermi 11-month survey catalogue. About 60% of sources were identified with counterparts in other wavelengths, most of which are extragalactic sources. Among them, XSS J12270-4859 stands out as a very peculiar Galactic source with unusual timing and spectral behaviours in the X-ray band. We aim to search for similar sources among the Fermi sources.	GALACTIC POINT SOURCES	4	C	NAOKI ISO		JAP	6	AO6	SEARCH FOR GAMMA-RAY BINARIES WITH A LOW-MASS COUNTERPART	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406014010/	Quick Look
401	PSR J1044-5737	161.1338	-57.616	160.63624	-57.35288	199.24967	-57.525785	286.57019106	1.16750605	109.1973	55542.2984259259	2010-12-12 07:09:44	55542.7292939815	2010-12-12 17:30:11	405013010	22.63	30	22.63	22.63	0	22.6358	1	1	0	1	1	0	0	21.9603	21.9603	37.2	0	PROCESSED	57554.3753125	2016-06-15 09:00:27	55917	2011-12-22 00:00:00	55550.9648148148	2010-12-20 23:09:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050047	Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.	GALACTIC POINT SOURCES	4	C	NOBUYUKI KAWAI		JAP	5	AO5	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405013010/	Quick Look
402	SGR 0501+4516	75.2625	45.3425	74.350391	45.26956	78.845173	22.471613	161.48747118	1.98100999	82.3996	55459.7272569444	2010-09-20 17:27:15	55460.9897337963	2010-09-21 23:45:13	405075010	59.7205	50	59.8085	59.8123	0	59.7205	3	2	0	2	1	0	0	52.9357	52.9357	109.0658	0	PROCESSED	57553.4903935185	2016-06-14 11:46:10	55287	2010-04-01 00:00:00	55470.1458449074	2010-10-01 03:30:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	5	AO5	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405075010/	Quick Look
403	AX J1620.7-4942	245.1985	-49.7112	244.261349	-49.592314	252.133944	-27.795213	333.72306976	0.21790295	274.6004	56158.5209027778	2012-08-19 12:30:06	56159.5245717593	2012-08-20 12:35:23	407020010	42.2062	40	44.2713	44.2744	0	42.2062	3	2	0	3	1	0	0	44.8052	44.8052	86.7119	0	PROCESSED	57606.89875	2016-08-06 21:34:12	56582	2013-10-17 00:00:00	56212.7789930556	2012-10-12 18:41:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070043	Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution.	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	7	AO7	ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407020010/	Quick Look
404	WR140	305.1374	43.8475	304.71526	43.688126	327.381123	60.483368	80.93293792	4.16074264	212.5272	56283.3528356482	2012-12-22 08:28:05	56284.2085300926	2012-12-23 05:00:17	407041010	54.7802	50	54.7962	54.7802	0	54.8042	3	2	0	3	1	0	0	52.3811	52.3811	73.92	0	PROCESSED	57608.3396990741	2016-08-08 08:09:10	56710	2014-02-22 00:00:00	56344.6961689815	2013-02-21 16:42:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071203	In the campaign observations of the prototypical colliding wind binary system WR 140 at its last periastron passage in 2009, Suzaku discovered an extremely hard and variable X-ray component. The current best explanation of its origin is inverse-Compton cooling of particles accelerated in the wind-wind collision shock, and if so this would be the first detection of non-thermal X-ray emission from any Wolf-Rayet system. However, other mechanisms cannot be excluded because the observed intensity was stronger than expected from the observed radio luminosity. We propose to re-observe WR 140 near apastron in 2012 with Suzaku to identify the emission mechanism which produces the hard component.	GALACTIC POINT SOURCES	4	C	KENJI HAMAGUCHI		USA	7	AO7	MEASURING EXTREMELY HARD X-RAY EMISSION FROM WR140 AT APASTRON	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407041010/	Quick Look
405	SGR 1806-20	272.1614	-20.4072	271.417079	-20.415895	272.018881	3.01842	9.99816367	-0.23801419	88.2521	57120.8242592593	2015-04-08 19:46:56	57122.7405324074	2015-04-10 17:46:22	408014010	70.8195	70	70.8195	74.7739	0	74.8169	2	2	0	3	0	0	0	0	0	0	0	PROCESSED	57618.0034143518	2016-08-18 00:04:55	57503	2016-04-25 00:00:00	57135.3828356482	2015-04-23 09:11:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080040	Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources.	GALACTIC POINT SOURCES	4	B	TERUAKI ENOTO		JAP	8	AO8	ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408014010/	Quick Look
406	V1223 SGR	283.7562	-31.163	282.951401	-31.227311	281.856338	-8.287095	4.95737746	-14.35200731	75.0006	56745.6297453704	2014-03-29 15:06:50	56746.5002430556	2014-03-30 12:00:21	408019010	29.3493	180	29.3893	29.3493	0	29.3967	1	1	0	2	1	0	0	26.131	26.131	75.192	1	PROCESSED	57614.1428703704	2016-08-14 03:25:44	57121	2015-04-09 00:00:00	56756.7522800926	2014-04-09 18:03:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080086	A 180-ks observation of the magnetic cataclysmic variable V1223 Sgr is proposed. By increasing the statistics by a factor of 4 compared to the existing 45-ks data, we investigate spin-phase dependent redshift of the iron fluorescent line, in particular its line center energy and equivalent width with smaller statistical errors than results of Hayashi et al. 2011. These parameters will provide geometrical configuration, or solid angle viewed from the post-shock region, of the pre-shock cool gas and the white dwarf reflecting surface. We use this information to make our Monte-Carlo simulator of magnetic CV more physically realistic and reliable in analyzing the high-resolution iron line profiles to be obtained with the ASTRO-H/SXS.	GALACTIC POINT SOURCES	4	B	TAKAYUKI YUASA		JAP	8	AO8	DEEP OBSERVATION OF THE MAGNETIC CATACLYSMIC VARIABLE V1223 SGR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408019010/	Quick Look
407	4U 1735-44	264.7467	-44.4484	263.834293	-44.420689	265.97323	-21.080234	346.05710105	-6.99533469	268.9985	56917.7849884259	2014-09-17 18:50:23	56918.9988194444	2014-09-18 23:58:18	408043020	10.1772	60	10.1772	10.2016	0	10.3047	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5500925926	2016-08-16 13:12:08	57626	2016-08-26 00:00:00	56940.6296064815	2014-10-10 15:06:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082017	We propose to observe the bursting low-mass X-ray binary 4U 1735-44 with Suzaku for a total exposure time of 60 ks. We plan to investigate the broad-band X-ray spectrum by performing a detailed spectroscopic and timing analysis in the energy range 0.4-100 keV. The main scientific aims of this observation are to detect and study the iron Kalpha line at 6.4-7 keV, simultaneously with the expected iron edge at 7-9 keV, emission lines at lower energy (such as S, Ar and Ca at 2.62 keV, 3.31 keV and 3.90 keV, respectively), and either a Compton reflection hump at 20-40 keV or a hard tail at energy above 25 keV (depending of the state of the source), thanks to the broad-band capabilities of Suzaku. This will allow to infer and probe the origin of these components, which is still debated.	GALACTIC POINT SOURCES	4	A	ELISE EGRON		EUR	8	AO8	BROAD-BAND SPECTRAL ANALYSIS AND STUDY OF THE DISK REFLECTION COMPONENT IN 4U 1735-44 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408043020/	Quick Look
408	GRO J1008-57	152.4313	-58.2999	151.999865	-58.053533	193.901629	-61.317749	282.99773034	-1.83149103	115.5012	56660.6548148148	2014-01-03 15:42:56	56661.5897569444	2014-01-04 14:09:15	408044010	15.3374	20	15.3374	15.3479	0	15.3374	3	3	0	3	1	0	0	22.1794	22.1794	55.0379	1	PROCESSED	57613.7393981482	2016-08-13 17:44:44	57040	2015-01-18 00:00:00	56679.7652662037	2014-01-22 18:21:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082019	We propose to observe the transient XRB GRO J1008−57 for 20 ks during an outburst in 2014 January after the currently ongoing giant outburst. The source exhibits regular outbursts once per orbit. Several of these outbursts have been observed in the past showing that the spectral shape remains constant between outbursts. Since we were able to improve the orbital ephemeris it is possible to predict future outbursts of the source. The source is currently (MJD 56245) exhibiting a giant type II outburst showing that the companion has ejected large amounts of material. We therefore propose to observe the system after this outburst to check for spectral and temporal changes and to study the iron line complex to derive the amount and ionization state of the material.	GALACTIC POINT SOURCES	4	A	INGO KREYKENBOHM		EUR	8	AO8	MEASURING THE RESIDUAL MATERIAL IN GRO J1008−57 AFTER THE GIANT OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408044010/	Quick Look
409	1RXSJ170856.9-235936	257.2347	-23.9931	256.473449	-23.929773	258.342614	-1.066908	359.58527393	9.56844908	95.2085	57099.2765625	2015-03-18 06:38:15	57099.6030324074	2015-03-18 14:28:22	409016010	15.3768	15	15.3768	15.3848	0	15.3768	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.8053703704	2016-08-17 19:19:44	57479	2016-04-01 00:00:00	57112.4072106482	2015-03-31 09:46:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090051	We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	B	HIDEYUKI MORI		JAP	9	AO9	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409016010/	Quick Look
410	SCT X-1	278.8604	-7.62	278.182699	-7.661262	279.107683	15.540839	24.33197703	0.06047842	260.9601	56940.5300810185	2014-10-10 12:43:19	56940.854375	2014-10-10 20:30:18	409033010	15.1616	50	15.1789	15.1776	0	15.1616	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6415625	2016-08-16 15:23:51	57373	2015-12-17 00:00:00	56979.4099421296	2014-11-18 09:50:19	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/ver3.0/409033010/	Quick Look
411	4U1700-37	255.9894	-37.8441	255.139416	-37.774677	258.577099	-14.956185	347.75582102	2.17172645	269.6945	53991.447662037	2006-09-13 10:44:38	53992.918912037	2006-09-14 22:03:14	401058010	81.4425	80	81.4569	81.4704	81.4425	81.4544	3	3	3	3	1	0	0	82.1093	82.1093	127.109	1	PROCESSED	57535.6097916667	2016-05-27 14:38:06	54526	2008-03-01 00:00:00	54053.5428240741	2006-11-14 13:01:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011135	The compact object in the massive X-ray binary 4U1700-37/HD153919 has been inferred to be a neutron star based on its spectral shape, but no pulsations have been observed. One possible explanation for the absence of observed pulsations is that the pulsed signal is beamed in directions other than our line of sight. This can be tested using Suzaku by searching for pulsations in the iron K line. This line is formed efficiently under almost all conditions of ionization and temperature, and so represents an X-ray bolometer which should respond to pulsed X-rays no matter where they are pointed. We plan to make such a search, and to probe the other properties of the wind and compact object in this system by observing with Suzaku for 80 ks away from eclipse.	GALACTIC POINT SOURCES	4	A	TIMOTHY KALLMAN		USA	1	AO1	IRON LINE VARIABILITY IN 4U1700-37	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401058010/	Quick Look
412	ALGOL	47.0831	40.8965	46.267674	40.705521	56.181748	22.363141	149.0355551	-14.93487401	244.4771	54167.6197222222	2007-03-08 14:52:24	54169.6132986111	2007-03-10 14:43:09	401093010	102.1642	105	102.1642	102.1642	0	102.1642	2	2	0	2	1	0	0	102.4729	102.4729	172.1928	1	PROCESSED	57537.6825810185	2016-05-29 16:22:55	54736	2008-09-27 00:00:00	54186.3983564815	2007-03-27 09:33:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012024	Stellar and solar coronae reveal high-energy phenomena including the presence of accelerated electrons, explosive dissipation of magnetic energy, and heating to extreme temperatures. Many of these processes are likely to be physically related. We propose to use Suzaku's suite of instruments to observe the interplay between thermal and non-thermal high-energy processes in the active, eclipsing binary Algol. Our prime objective is the observation of hard X-rays above 10 keV, but also the appearance of an Fe fluorescence line that could be induced either by irradiation from flaring plasma or by electron beams. These models can be distinguished by correlating the emission with nonthermal hard X-rays as possibly detected by the HXD.	GALACTIC POINT SOURCES	4	C	MANUEL GUEDEL		EUR	1	AO1	A SYNOPTIC VIEW OF HIGH-ENERGY PHENOMENA IN THE CORONA OF ALGOL	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401093010/	Quick Look
413	SERPENS X-1	279.9934	5.0285	279.376671	4.981655	281.288405	28.078275	36.11311789	4.83561165	256.1423	54032.2853819444	2006-10-24 06:50:57	54033.2259143518	2006-10-25 05:25:19	401048010	37.1578	37	37.1578	37.2698	37.2058	37.1658	2	1	2	2	1	0	0	31.0695	31.0695	81.2399	2	PROCESSED	57535.9734722222	2016-05-27 23:21:48	54526	2008-03-01 00:00:00	54056.4719328704	2006-11-17 11:19:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011113	The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme.	GALACTIC POINT SOURCES	4	B	JON MILLER		USA	1	AO1	A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401048010/	Quick Look
414	4U 1636-536	250.2273	-53.7542	249.230886	-53.657708	256.461437	-31.236858	332.91122007	-4.81806999	91.2447	54153.2955787037	2007-02-22 07:05:38	54154.3544560185	2007-02-23 08:30:25	401050020	40.096	38	40.096	40.104	0	40.096	2	1	0	2	1	0	0	35.55	35.55	91.4779	0	PROCESSED	57537.4821990741	2016-05-29 11:34:22	54525	2008-02-29 00:00:00	54158.392037037	2007-02-27 09:24:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011117	Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.	GALACTIC POINT SOURCES	4	A	JEROEN HOMAN		USA	1	AO1	THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050020/	Quick Look
415	HER X-1	254.4925	35.2707	254.041525	35.346159	246.065216	57.427888	58.06565994	37.48335671	250.2455	55468.7003356482	2010-09-29 16:48:29	55469.2258912037	2010-09-30 05:25:17	405058020	24.303	20	24.303	24.3223	0	24.4677	2	2	0	1	1	0	0	22.4837	22.4837	45.4059	0	PROCESSED	57553.5917476852	2016-06-14 14:12:07	55848	2011-10-14 00:00:00	55482.4726967593	2010-10-13 11:20:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052001	We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity?	GALACTIC POINT SOURCES	4	B	R DIGER STAUBERT		EUR	5	AO5	VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405058020/	Quick Look
416	IGRJ16493-4348	252.3173	-43.8652	251.422595	-43.77854	256.400238	-21.254215	341.31911758	0.57823277	287.444	54013.8822916667	2006-10-05 21:10:30	54014.4204166667	2006-10-06 10:05:24	401054010	21.1998	20	21.2158	21.2158	21.1998	21.2078	3	3	3	3	1	0	0	20.2197	20.2197	46.4639	1	PROCESSED	57535.7818634259	2016-05-27 18:45:53	54695	2008-08-17 00:00:00	54025.4796412037	2006-10-17 11:30:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011132	INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	1	AO1	HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401054010/	Quick Look
417	SGR 1806-20	272.166	-20.4729	271.421316	-20.481616	272.022208	2.952663	9.94279657	-0.27364584	269.9473	53987.9261921296	2006-09-09 22:13:43	53989.1668287037	2006-09-11 04:00:14	401092010	48.9155	50	48.9155	48.9235	48.9315	48.9315	1	1	1	1	1	0	0	55.4085	55.4085	107.1759	1	PROCESSED	57535.5272453704	2016-05-27 12:39:14	54526	2008-03-01 00:00:00	54021.1112615741	2006-10-13 02:40:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012017	The soft gamma-ray repeater SGR 1806-20 has recently emitted the most powerful giant flare ever observed from these sources. This probably involved a large scale restructuring of the magnetosphere, leading to observable variations in the properties of its persistent emission, from IR to hard X-rays. We propose to observe SGR 1806-20 with Suzaku considering the unique opportunity offered by this satellite to study the spectrum of this source simultaneously both in the soft and hard X-ray bands. We also suggest to coordinate this observation with a simultaneous XMM-Newton one, in order to obtain a significantly better determination of the broad band spectral parameters.	GALACTIC POINT SOURCES	4	B	SANDRO MEREGHETTI		EUR	1	AO1	COORDINATED SUZAKU AND XMM-NEWTON OBSERVATIONS OF SGR 1806-20 AFTER THE GIANT FLARE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401092010/	Quick Look
418	CYG X-1	299.5792	35.2719	299.109639	35.135474	313.688752	54.318748	71.39034122	3.11120593	84.3565	54220.8163657407	2007-04-30 19:35:34	54221.783587963	2007-05-01 18:48:22	402072010	45.3204	30	45.3204	45.3284	0	45.3204	2	1	0	2	1	0	0	40.1873	40.1873	83.566	2	PROCESSED	57538.518275463	2016-05-30 12:26:19	54773	2008-11-03 00:00:00	54228.1718518518	2007-05-08 04:07:28	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/ver3.0/402072010/	Quick Look
419	SWIFT J1753.5-0127	268.3714	-1.4588	267.723576	-1.449322	268.234398	21.971701	24.89300861	12.1795145	261.3846	54362.8585185185	2007-09-19 20:36:16	54365.4377777778	2007-09-22 10:30:24	402088010	94.6005	93	94.6085	94.6165	0	94.6005	2	2	0	2	1	0	0	81.739	81.739	222.836	3	PROCESSED	57540.1123842593	2016-06-01 02:41:50	54743	2008-10-04 00:00:00	54371.6366319444	2007-09-28 15:16:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021147	While the spectrally hard state represents the most common mode of accretion in black hole X-ray binaries, the nature of its accretion flow is poorly understood. We recently discovered cool accretion disks extending close to the innermost stable circular orbit in the hard states of two black hole transients. Such disks could give rise to strong reflection features, but instead these are weak or not detected. We propose a 70 ks Suzaku observation of Swift J1753.5-0127 (one of the two transients), which is currently in a prolonged hard state. Our goal is to put tight constraints on the strength of the reflection features and increase our understanding of the geometry of the spectrally hard component. Understanding accretion onto compact objects is fundamental to NASA's "SEU" theme.	GALACTIC POINT SOURCES	4	A	JEROEN HOMAN		USA	2	AO2	CONSTRAINING REFLECTION FEATURES IN THE HARD STATE OF BLACK HOLE X-RAY BINARIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402088010/	Quick Look
420	MARS-P18	103.5869	25.0943	102.819218	25.15788	102.294706	2.231395	190.58743765	11.74868918	298.2592	54560.7434837963	2008-04-04 17:50:37	54560.8264351852	2008-04-04 19:50:04	403006180	1.8618	100	1.8618	1.8618	0	1.8618	1	1	0	1	1	0	0	1.9396	1.9396	7.1539	0	PROCESSED	57542.0705555556	2016-06-03 01:41:36	54953	2009-05-02 00:00:00	54578.0530555556	2008-04-22 01:16:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006180/	Quick Look
421	TAU SCO	248.9733	-28.218	248.193759	-28.116325	251.450612	-6.120226	351.53478934	12.80506422	280.0312	54729.4179398148	2008-09-20 10:01:50	54729.7578009259	2008-09-20 18:11:14	403034040	13.9711	10	13.9711	13.9711	0	13.9711	2	2	0	2	1	0	0	12.8912	12.8912	29.35	0	PROCESSED	57543.857974537	2016-06-04 20:35:29	55148	2009-11-13 00:00:00	54780.4954050926	2008-11-10 11:53:23	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/ver3.0/403034040/	Quick Look
422	IGR J00234+6141	5.7092	61.7549	5.020335	61.477793	39.893501	52.142885	119.55446517	-0.92914674	80.286	55372.004375	2010-06-25 00:06:18	55373.2397569445	2010-06-26 05:45:15	405022010	81.88	80	81.88	81.88	0	81.88	2	2	0	2	1	0	0	70.0364	70.0364	106.6979	1	PROCESSED	57552.4371759259	2016-06-13 10:29:32	55780	2011-08-07 00:00:00	55414.1791666667	2010-08-06 04:18:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050059	Suzaku discovery of the first white dwarf pulsar, AE Aqr (Terada et.al 2008) had a great impact on the studies of the cosmic-ray origin, since white dwarfs were not recognized as a particle accelerator. The next step is to check whether this phenomenon is common or not. In order to search for the second white dwarf pulsar, we picked up hard objects among the INTEGRAL and Swift sample, and propose the Suzaku observation of the best two objects, V2487 Oph and IGRJ00234+6141.	GALACTIC POINT SOURCES	4	A	YUKIKATSU TERADA		JAP	5	AO5	SEARCH FOR NON-THERMAL EMISSION FROM HARD WHITE DWARFS WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405022010/	Quick Look
423	XSS J12270-4859	187.002	-48.8936	186.3245	-48.617009	209.763835	-41.252243	298.97017898	13.79783482	315.9792	54686.9674421296	2008-08-08 23:13:07	54687.6480787037	2008-08-09 15:33:14	403029010	29.6232	30	29.6232	29.6232	0	29.6232	2	2	0	2	1	0	0	34.58	34.58	58.7919	0	PROCESSED	57543.2069907407	2016-06-04 04:58:04	55073	2009-08-30 00:00:00	54707.1730208333	2008-08-29 04:09:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030140	Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	3	AO3	IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403029010/	Quick Look
424	TAU SCO	248.9731	-28.2173	248.193563	-28.115624	251.450335	-6.119558	351.53521528	12.80565459	288.7028	54717.0750115741	2008-09-08 01:48:01	54717.3752777778	2008-09-08 09:00:24	403034020	14.5215	10	14.5295	14.5215	0	14.5375	1	1	0	1	1	0	0	9.6524	9.6524	25.9359	1	PROCESSED	57543.7784606482	2016-06-04 18:40:59	55148	2009-11-13 00:00:00	54780.6118171296	2008-11-10 14:41:01	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/ver3.0/403034020/	Quick Look
425	YY MEN	74.6207	-75.281	75.005816	-75.353979	292.803657	-80.004198	287.41045099	-33.23069192	7.2587	54996.0772916667	2009-06-14 01:51:18	54998.5606365741	2009-06-16 13:27:19	404036010	106.9498	100	106.9578	106.9578	0	106.9498	2	2	0	2	1	0	0	104.0902	104.0902	214.5398	0	PROCESSED	57547.6240393518	2016-06-08 14:58:37	55378	2010-07-01 00:00:00	55008.2997106482	2009-06-26 07:11:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041202	The single K giant YY Men is one of the most active stars within 300 pc of the Sun, having produced 2 of the most powerful radio flares and 1 of the most powerful and long-duration optical flares ever detected. Its corona is one of the hottest and brightest known, with a typical X-ray luminosity of 32.0-32.5 (log erg/s) which most other cool stars only reach during major flares. We propose to obtain a 100-ksec observation of this hyperactive star to get a high S/N XIS exposure of its spectrum, particularly in the 5-10 keV region in which the XIS excels. We will study the He- and H-like Fe lines, search for 6.4 keV fluorescent emission, search for the presence of ultrahigh temperature and nonthermal spectral components, and look for correlations with simultaneous ATCA radio observations.	GALACTIC POINT SOURCES	4	B	STEPHEN DRAKE		USA	4	AO4	THE EXTREME CORONAL PROPERTIES OF THE HYPERACTIVE K GIANT YY MEN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404036010/	Quick Look
426	IGR J08408-4503	130.2449	-45.0216	129.817019	-44.842502	154.934869	-59.72126	264.03123634	-1.90203871	133.4432	55176.7452199074	2009-12-11 17:53:07	55179.5002199074	2009-12-14 12:00:19	404070010	92.566	100	92.646	92.566	0	92.63	2	2	0	2	1	0	0	69.4344	69.4344	237.9898	2	PROCESSED	57549.8697222222	2016-06-10 20:52:24	55567	2011-01-06 00:00:00	55200.3941550926	2010-01-04 09:27:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042007	We propose a 100 ks Suzaku observation of a Supergiant Fast X-ray Transient (SFXT) displaying periodic outbursts, IGRJ08408-4503, with the main aim of searching for cyclotron lines in its spectrum.This would be the first direct measurement of the neutron star magnetic field in this recently discovered class of HMXBs, and would be crucial in discriminating between different models for the outburst mechanisms, involving highly magnetized neutron stars (1E14 G) versus more typical magnetic fields of 1E12 G.The source is a SFXT displaying recurrent outbursts on short timescales (flaring every about 11 and 24 days).Because in most SFXTs the outbursts are not predictable, fast and difficult to observe,the SFXT we are proposing is a key system to understand the physical properties of this class.	GALACTIC POINT SOURCES	4	C	LARA SIDOLI		EUR	4	AO4	SEARCH FOR CYCLOTRON LINES IN THE X-RAY SPECTRUM OF THE SUPERGIANT FAST X-RAY TRANSIENT IGRJ08408-4503	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404070010/	Quick Look
427	CYGNUS X-1	299.5964	35.2723	299.126812	35.135802	313.711652	54.314398	71.39800953	3.09942804	95.8123	54924.0537384259	2009-04-03 01:17:23	54924.5654282407	2009-04-03 13:34:13	404075010	15.3091	300	15.3091	15.3188	0	15.3108	2	1	0	2	1	0	0	15.5374	15.5374	44.2039	1	PROCESSED	57546.0113425926	2016-06-07 00:16:20	54922	2009-04-01 00:00:00	54949.4917824074	2009-04-28 11:48:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075010/	Quick Look
428	EMS01095	252.3381	-45.0256	251.43287	-44.939011	256.578669	-22.402784	340.43907916	-0.17827348	87.5534	55603.1544328704	2011-02-11 03:42:23	55603.7613310185	2011-02-11 18:16:19	405027010	20.9332	20	20.9344	20.9344	0	20.9332	2	2	0	2	1	0	0	16.9762	16.9762	52.4319	0	PROCESSED	57600.9093055556	2016-07-31 21:49:24	55983	2012-02-26 00:00:00	55617.4127430556	2011-02-25 09:54:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050104	Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV.	GALACTIC POINT SOURCES	4	A	YASUYUKI TANAKA		JAP	5	AO5	SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405027010/	Quick Look
429	CYGNUS X-1	299.5337	35.2545	299.064105	35.118267	313.618737	54.314854	71.35609035	3.13386262	50.0944	54980.4956712963	2009-05-29 11:53:46	54981.0586226852	2009-05-30 01:24:25	404075100	28.7845	300	28.7845	28.7845	0	28.7845	1	1	0	1	1	0	0	25.7389	25.7389	48.6319	1	PROCESSED	57546.7292476852	2016-06-07 17:30:07	54922	2009-04-01 00:00:00	54994.3872800926	2009-06-12 09:17:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075100/	Quick Look
430	CYGNUS X-1	299.5272	35.2497	299.057586	35.113495	313.607401	54.312117	71.34921869	3.1358965	44.7834	54986.8208333333	2009-06-04 19:42:00	54987.3356944444	2009-06-05 08:03:24	404075120	16.8733	300	16.8813	16.8894	0	16.8733	2	1	0	2	1	0	0	6.7647	6.7647	44.4779	1	PROCESSED	57547.4806018518	2016-06-08 11:32:04	54922	2009-04-01 00:00:00	55001.0163078704	2009-06-19 00:23:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075120/	Quick Look
431	1RXS J1708-4009	257.2032	-40.2034	256.333623	-40.139657	259.789477	-17.214031	346.44001394	-0.00188973	266.4021	55066.6841203704	2009-08-23 16:25:08	55067.9466898148	2009-08-24 22:43:14	404080010	60.8869	60	60.8869	60.8949	0	60.9046	3	2	0	2	1	0	0	51.5313	51.5313	109.0758	1	PROCESSED	57548.350150463	2016-06-09 08:24:13	54922	2009-04-01 00:00:00	55078.1751851852	2009-09-04 04:12:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	4	AO4	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404080010/	Quick Look
432	HD125599	215.4515	-48.0762	214.633471	-47.848202	230.117069	-31.899698	318.15137849	12.10713587	289.1653	55414.6760069444	2010-08-06 16:13:27	55415.1571990741	2010-08-07 03:46:22	405030010	31.048	30	31.056	31.056	0	31.048	1	1	0	1	1	0	0	24.8599	24.8599	41.5679	0	PROCESSED	57552.8615277778	2016-06-13 20:40:36	55793	2011-08-20 00:00:00	55427.1753819444	2010-08-19 04:12:33	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050116	Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	5	AO5	QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405030010/	Quick Look
433	GX 1+4	263.0071	-24.816	262.238766	-24.780248	263.643916	-1.529018	1.87675865	4.75818757	273.1727	55471.2801273148	2010-10-02 06:43:23	55473.5140509259	2010-10-04 12:20:14	405077010	99.67	100	99.6704	99.67	0	99.6704	3	2	0	2	1	0	0	96.5259	96.5259	192.6091	0	PROCESSED	57553.6626967593	2016-06-14 15:54:17	55287	2010-04-01 00:00:00	55487.4199537037	2010-10-18 10:04:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	5	AO5	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405077010/	Quick Look
434	T PYXIDIS	136.1704	-32.3688	135.652133	-32.168809	152.023797	-46.371088	257.19727302	9.71237496	121.9943	56266.272662037	2012-12-05 06:32:38	56268.8695486111	2012-12-07 20:52:09	407048010	86.676	100	86.676	86.676	0	86.676	2	2	0	2	1	0	0	73.6118	73.6118	224.3579	4	PROCESSED	57608.249525463	2016-08-08 05:59:19	56660	2014-01-03 00:00:00	56291.8230787037	2012-12-30 19:45:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071213	We propose a 100 ks observation of the classical nova remnant in the accreting binary system T Pyxidis using Suzaku. T Pyxidis is a system which causes a cycle of classical nova outbursts in a decade time scale. Shocks might occur in the ejecta, and X-rays were detected from its spatially-resolved expanding shell like a miniature supernova remnant. The immediate purposes of this program are (1) to derive the X-ray flux and luminosity after its last outburst in 2011, (2) to diagnose plasma temperature deeply, and (3) to obtain the second sample of non-thermal X-ray emission from classical nova remnants. The target is a remarkable newly discovered candidate of cosmic-ray acceleration sites, and a successful detection of non-thermal X-rays provides a new view of cosmic-ray origins.	GALACTIC POINT SOURCES	4	C	DAI TAKEI		USA	7	AO7	COSMIC-RAYS FROM MINIATURE SUPERNOVA REMNANTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407048010/	Quick Look
435	HERCULES X-1	254.4605	35.3288	254.009904	35.404408	245.996246	57.479663	58.13264186	37.51848299	268.3999	56192.1811342593	2012-09-22 04:20:50	56192.781412037	2012-09-22 18:45:14	407051020	22.6094	20	22.6094	22.6094	0	22.6094	3	2	0	2	1	0	0	20.1787	20.1787	51.836	1	PROCESSED	57607.16	2016-08-07 03:50:24	56590	2013-10-25 00:00:00	56218.5726967593	2012-10-18 13:44:41	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/ver3.0/407051020/	Quick Look
436	1RXSJ171405.2-202747	258.5195	-20.4586	257.777244	-20.401416	259.232449	2.554431	3.21945841	10.61986264	93.18	57079.8384027778	2015-02-26 20:07:18	57080.0974652778	2015-02-27 02:20:21	409012010	10.9777	10	10.9777	11.0017	0	10.9937	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.6641319444	2016-08-17 15:56:21	57458	2016-03-11 00:00:00	57091.4587847222	2015-03-10 11:00:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090051	We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	B	HIDEYUKI MORI		JAP	9	AO9	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409012010/	Quick Look
437	1RXSJ165739.1-294946	254.4116	-29.828	253.617619	-29.751315	256.402928	-7.119224	353.32761408	8.10480043	98.1097	57103.7733333333	2015-03-22 18:33:36	57104.2294328704	2015-03-23 05:30:23	409014010	17.2255	12	17.2255	17.2575	0	17.2335	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.8394212963	2016-08-17 20:08:46	57486	2016-04-08 00:00:00	57119.4211458333	2015-04-07 10:06:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090051	We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	B	HIDEYUKI MORI		JAP	9	AO9	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409014010/	Quick Look
438	AB DOR	82.2881	-65.4658	82.252574	-65.503277	15.679222	-86.688003	275.31538375	-33.00189818	204.2849	54108.0647569444	2007-01-08 01:33:15	54109.4724421296	2007-01-09 11:20:19	401031020	49.0965	45	49.0965	49.0965	0	49.0965	2	2	0	2	1	0	0	44.9611	44.9611	121.6199	2	PROCESSED	57536.5000578704	2016-05-28 12:00:05	54502	2008-02-06 00:00:00	54133.0127083333	2007-02-02 00:18:18	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011021	We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku.	GALACTIC POINT SOURCES	4	B	MARC AUDARD		USA	1	AO1	NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401031020/	Quick Look
439	1RXS J213344.1+51072	323.4354	51.1973	323.001109	50.974362	356.300054	59.716219	94.50909334	-0.42447705	94.0452	53854.2853009259	2006-04-29 06:50:50	53856.2501736111	2006-05-01 06:00:15	401038010	81.9241	80	81.9241	81.9241	81.9241	81.9241	2	2	2	2	1	0	0	62.8881	62.8881	169.7261	3	PROCESSED	57533.6330671296	2016-05-25 15:11:37	54391	2007-10-18 00:00:00	53908.1887962963	2006-06-22 04:31:52	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011102	Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber.	GALACTIC POINT SOURCES	4	A	KOJI MUKAI		USA	1	AO1	BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401038010/	Quick Look
440	V893 SCO	243.8144	-28.6275	243.038085	-28.502934	247.008203	-7.251726	348.06577336	15.88028883	274.6746	53973.4024189815	2006-08-26 09:39:29	53974.056412037	2006-08-27 01:21:14	401041010	18.4978	20	18.4978	18.4978	18.4978	18.4978	2	2	2	2	1	0	0	16.1403	16.1403	56.482	0	PROCESSED	57535.3695601852	2016-05-27 08:52:10	54526	2008-03-01 00:00:00	54053.4763888889	2006-11-14 11:26:00	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011103	The RXTE All-Sky Slew Survey (XSS) catalog, containing 294 objects detected in the 3-20 keV sky, is of great potential use for a variety of purposes. Included in this catalog are two sources identified with lesser known dwarf novae, V893 Sco and SS Aur. Although these are known to be soft X-ray sources from the ROSAT All-sky Survey, there has never been a pointed observation with an imaging X-ray telescope of either object. Here I propose short Suzaku observations of V893 Sco and SS Aur to check the reliability of XSS fluxes, hence that of the luminosity functions derived from the XSS catalog. In addition, such observations serve as a pilot study to determine if these individual dwarf novae may merit further in-depth X-ray studies.	GALACTIC POINT SOURCES	4	B	KOJI MUKAI		USA	1	AO1	CONFIRMING THE IDENTIFICATION OF RXTE ALL-SKY SLEW SURVEY SOURCES WITH DWARF NOVAE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401041010/	Quick Look
441	4U 1636-536	250.2277	-53.7538	249.23129	-53.65731	256.461636	-31.236425	332.91167841	-4.81798429	93.2445	54186.4802777778	2007-03-27 11:31:36	54187.3043287037	2007-03-28 07:18:14	401050040	32.1304	38	32.1304	32.1384	0	32.1304	2	1	0	2	1	0	0	27.7842	27.7842	71.1779	1	PROCESSED	57538.0141782407	2016-05-30 00:20:25	54695	2008-08-17 00:00:00	54209.541412037	2007-04-19 12:59:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011117	Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.	GALACTIC POINT SOURCES	4	A	JEROEN HOMAN		USA	1	AO1	THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050040/	Quick Look
442	4U 1822-37	276.4461	-37.1042	275.595774	-37.133404	275.279951	-13.781506	356.85149319	-11.29112534	258.4537	54010.4563888889	2006-10-02 10:57:12	54011.5189699074	2006-10-03 12:27:19	401051010	37.7434	40	37.7682	37.7682	37.7434	37.7434	2	2	2	2	1	0	0	33.1785	33.1785	91.8059	0	PROCESSED	57535.7615393518	2016-05-27 18:16:37	54695	2008-08-17 00:00:00	54024.6539814815	2006-10-16 15:41:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011121	We propose a 40 ks observation of the accretion disk corona source 4U 1822-37. Despite repeated observations over the years and even excellent high-resolution data from the Chandra Observatory, the nature and origin of the corona and even the source of the Fe K fluorescence emission remains controversial. The spectral resolution of the XIS and the broad-band coverage provided by the combined XIS and HXD instruments make Suzaku uniquely suited to a definitive measurement. Determining the physical conditions in this source is particularly interesting. Because of its geometry 4U 1822-37 is a link between x-ray binaries and AGN, and an therefore serve as a laboratory for studying accretion processes throughout the universe.	GALACTIC POINT SOURCES	4	B	JEAN COTTAM		USA	1	AO1	ACCRETION PHYSICS IN THE ADC SOURCE 4U 1822-37	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401051010/	Quick Look
443	HESSJ1813-178	273.3946	-17.7704	272.66469	-17.785118	273.238499	5.632147	12.87014503	0.01155473	90.9367	54160.8999768518	2007-03-01 21:35:58	54162.2814699074	2007-03-03 06:45:19	401101010	63.8391	65	63.8471	63.8391	0	63.8471	2	2	0	2	1	0	0	57.7561	57.7561	119.3519	1	PROCESSED	57537.5358449074	2016-05-29 12:51:37	54736	2008-09-27 00:00:00	54167.6346990741	2007-03-08 15:13:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014214	Radio and X-ray observations towards the VHE gamma-ray source HESS J1813-178, initially dubbed being a dark accelerator , suggested its association with a SNR. However, a recent XMM observation confirmed earlier ASCA findings of an extended, center-filled X-ray source, not resembling the contours of the radio-detected SNR. We propose hard X-ray observations to investigate the alternatively plerionic origin of HESS J1813-178, given the wide spectral coverage possible by XIS/HXD. This will clarify the discrepancy between ASCA and recent INTEGRAL data. Constructing a valid spectral energy distribution will enable us to constrain the age and field strength of the particle accelerator powering the synchrotron emission and accurately model the radiation processes up to VHE energies.	GALACTIC POINT SOURCES	4	B	OLAF REIMER	KEN EBISAWA	USJ	1	AO1	IS THE ASSOCIATION OF HESS J1813-178/SNR G12.8-0.0 CONCEALING ITS TRUE PLERIONIC NATURE?	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401101010/	Quick Look
444	1RXSJ174459.5-172640	266.2467	-17.4406	265.51875	-17.420611	266.390507	5.953243	9.76958181	6.08973572	101.0461	54555.6304050926	2008-03-30 15:07:47	54556.5834953704	2008-03-31 14:00:14	402003010	43.5793	40	43.5953	43.5793	0	43.6033	1	1	0	1	1	0	0	29.5916	29.5916	82.3439	1	PROCESSED	57541.9975462963	2016-06-02 23:56:28	54937	2009-04-16 00:00:00	54570.1529282407	2008-04-14 03:40:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020015	We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, which were detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the Suzaku fine spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test acrretion disk theories at intermediate mass accretion rates.	GALACTIC POINT SOURCES	4	C	HIDEYUKI MORI		JAP	2	AO2	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402003010/	Quick Look
445	U SCO	245.629	-17.8143	244.907277	-17.697813	246.808051	3.686286	357.72199881	21.90970563	93.274	55236.514375	2010-02-09 12:20:42	55237.1668865741	2010-02-10 04:00:19	404018020	28.9369	20	28.9369	28.9369	0	28.9369	2	2	0	2	1	0	0	18.3288	18.3288	56.3699	0	PROCESSED	57550.5565393518	2016-06-11 13:21:25	55619	2011-02-27 00:00:00	55251.1498611111	2010-02-24 03:35:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040057	We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each.	GALACTIC POINT SOURCES	4	A	DAI TAKEI		JAP	4	AO4-TOO	TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404018020/	Quick Look
446	PSR B1259-63	195.6821	-63.8856	194.892558	-63.616964	227.728655	-50.936167	304.1741357	-1.04108664	280.935	54288.622025463	2007-07-07 14:55:43	54289.062662037	2007-07-08 01:30:14	402014010	21.8634	20	21.8714	21.8634	0	21.8714	1	1	0	1	1	0	0	26.86	26.86	38.0639	1	PROCESSED	57539.1256481482	2016-05-31 03:00:56	54696	2008-08-18 00:00:00	54328.4884722222	2007-08-16 11:43:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014010/	Quick Look
447	HD432	2.3072	59.1394	1.650501	58.861236	35.115755	51.206006	117.5327944	-3.28915956	247.7181	54469.7038310185	2008-01-04 16:53:31	54470.5154513889	2008-01-05 12:22:15	402034010	38.2406	40	38.2486	38.2406	0	38.2486	2	2	0	2	1	0	0	35.0503	35.0503	70.12	1	PROCESSED	57540.9911574074	2016-06-01 23:47:16	54908	2009-03-18 00:00:00	54483.4635532407	2008-01-18 11:07:31	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021016	Suzaku XIS spectra of three "X-ray deficient" Hertzsprung gap giants will explore why they display anomalous coronal behavior compared with cooler giants only slightly further advanced in their evolution. The apparent sharp transition in coronal properties on the way to helium flash might be caused by disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. A key discriminator is the coronal energy distribution, especially enhanced and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution; all three have supporting high resolution UV spectra. Expanding the sample of high quality, high energy information on this key class of objects is essential for probing their odd behavior.	GALACTIC POINT SOURCES	4	C	THOMAS AYRES		USA	2	AO2	ANOMALOUS CORONAE OF HERTZSPRUNG GAP GIANTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402034010/	Quick Look
448	SW UMA	129.1769	53.4845	128.242011	53.658568	116.840982	33.632115	164.80593722	36.96002764	98.2716	54410.2367708333	2007-11-06 05:40:57	54410.6252199074	2007-11-06 15:00:19	402044010	16.8991	20	16.9071	16.8991	0	16.9071	1	1	0	1	1	0	0	13.8969	13.8969	33.5519	1	PROCESSED	57540.4388194444	2016-06-01 10:31:54	54784	2008-11-14 00:00:00	54417.2697569444	2007-11-13 06:28:27	3.0.22.43	3	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/ver3.0/402044010/	Quick Look
449	GX17+2	274.0098	-14.0991	273.299204	-14.116851	273.930842	9.286846	16.37876929	1.24433559	268.3778	54370.5988078704	2007-09-27 14:22:17	54371.2502199074	2007-09-28 06:00:19	402050020	23.0117	20	23.0197	23.0258	0	23.0117	3	2	0	3	1	0	0	19.0488	19.0488	56.276	0	PROCESSED	57540.1139351852	2016-06-01 02:44:04	54769	2008-10-30 00:00:00	54402.3511921296	2007-10-29 08:25:43	3.0.22.43	2	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/ver3.0/402050020/	Quick Look
450	2S 0921-630	140.6643	-63.2995	140.374106	-63.084565	195.141929	-68.892072	281.84516955	-9.33669084	18.1705	54342.4079166667	2007-08-30 09:47:24	54343.5134722222	2007-08-31 12:19:24	402058010	45.6937	40	45.6937	45.6937	0	45.6937	2	2	0	2	1	0	0	43.3463	43.3463	95.4998	2	PROCESSED	57539.9018981482	2016-05-31 21:38:44	54724	2008-09-15 00:00:00	54356.2760763889	2007-09-13 06:37:33	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/ver3.0/402058010/	Quick Look
451	IGR J00370+6122	9.2836	61.3722	8.564252	61.097243	41.619526	50.769336	121.21895683	-1.4519667	87.6081	54273.499849537	2007-06-22 11:59:47	54274.230775463	2007-06-23 05:32:19	402064010	34.9089	30	35.3844	35.4004	0	34.9089	2	2	0	2	1	0	0	33.7926	33.7926	63.1419	2	PROCESSED	57637.5249652778	2016-09-06 12:35:57	54695	2008-08-17 00:00:00	54322.4714236111	2007-08-10 11:18:51	3.0.22.44	3	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/ver3.0/402064010/	Quick Look
452	4U 1907+09	287.4001	9.8965	286.805564	9.814618	290.343315	32.116545	43.79892996	0.51344636	85.3836	54209.4191666667	2007-04-19 10:03:36	54211.2612731482	2007-04-21 06:16:14	402067010	80.6283	65	80.6283	80.6363	0	80.6363	2	2	0	2	1	0	0	73.2685	73.2685	159.1479	2	PROCESSED	57538.4515393518	2016-05-30 10:50:13	54702	2008-08-24 00:00:00	54216.2674189815	2007-04-26 06:25:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021123	The HMXB 4U 1907+09 shows a rich phenomenology: two cyclotron lines, an uncommonly weak iron line, intermittent X-ray fading, and a recent torque reversal. Compared to other persistent supergiant X-ray pulsars it has been less well observed, although it is a prime target to study the interaction of the neutron star's X-rays with the stellar wind and the accretion column. The latter has been confirmed by our 60ks AO1 observation which allowed for the first detection of a soft excess below 2keV as well as the determination of the paramters of the fundamental cyclotron line with unprecedented accuracy. Due to an unusually low source state during the AO1 exposure, however, an additional observation of 65ks is needed to perform the first phase resolved analysis of this interesting source.	GALACTIC POINT SOURCES	4	B	KATJA POTTSCHMIDT		USA	2	AO2	THE BROAD BAND SPECTRUM OF 4U 1907+09	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402067010/	Quick Look
453	MARS-P6	103.0844	25.143	102.316186	25.2042	101.836831	2.238113	190.34808199	11.3557719	298.0743	54559.7434375	2008-04-03 17:50:33	54559.8265972222	2008-04-03 19:50:18	403006060	1.939	100	1.939	1.939	0	1.939	1	1	0	1	1	0	0	1.8046	1.8046	7.1819	0	PROCESSED	57542.0435416667	2016-06-03 01:02:42	54953	2009-05-02 00:00:00	54577.1376388889	2008-04-21 03:18:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006060/	Quick Look
454	MARS-P7	103.127	25.1401	102.358824	25.201502	101.875529	2.238706	190.36726484	11.38956433	298.0907	54559.8267476852	2008-04-03 19:50:31	54559.9029861111	2008-04-03 21:40:18	403006070	2.5028	100	2.5139	2.5108	0	2.5028	1	1	0	1	1	0	0	1.6506	1.6506	6.584	0	PROCESSED	57542.0488310185	2016-06-03 01:10:19	54953	2009-05-02 00:00:00	54577.1486342593	2008-04-21 03:34:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006070/	Quick Look
455	MARS-P12	103.3358	25.1148	102.567873	25.177192	102.066233	2.230736	190.47148034	11.55063865	298.1645	54560.2434837963	2008-04-04 05:50:37	54560.3266666667	2008-04-04 07:50:24	403006120	3.455	100	3.455	3.455	0	3.455	1	1	0	1	1	0	0	2.678	2.678	7.1759	0	PROCESSED	57542.0566782407	2016-06-03 01:21:37	54953	2009-05-02 00:00:00	54577.1789467593	2008-04-21 04:17:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006120/	Quick Look
456	YY DRA	175.8686	71.6187	175.161968	71.896164	128.299312	59.497013	130.35712902	44.51671754	282.0676	54632.7758217593	2008-06-15 18:37:11	54633.4098842593	2008-06-16 09:50:14	403022010	29.1851	30	29.1851	29.1851	0	29.1851	2	2	0	2	1	0	0	27.4743	27.4743	54.7779	1	PROCESSED	57542.8240509259	2016-06-03 19:46:38	55013	2009-07-01 00:00:00	54644.1517592593	2008-06-27 03:38:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030107	We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.	GALACTIC POINT SOURCES	4	C	TAKAYUKI YUASA		JAP	3	AO3	SURVEY OBSERVATION OF INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403022010/	Quick Look
457	TV COL	82.3326	-32.8641	81.870324	-32.902382	78.445337	-55.999473	236.83580562	-30.63495041	295.9146	54573.7555555556	2008-04-17 18:08:00	54574.6668634259	2008-04-18 16:00:17	403023010	35.8367	40	35.8367	35.8367	0	35.8367	2	2	0	2	1	0	0	30.1023	30.1023	78.7299	0	PROCESSED	57542.3393055556	2016-06-03 08:08:36	54953	2009-05-02 00:00:00	54587.0666550926	2008-05-01 01:35:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030107	We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.	GALACTIC POINT SOURCES	4	C	TAKAYUKI YUASA		JAP	3	AO3	SURVEY OBSERVATION OF INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403023010/	Quick Look
458	HD72779	128.8308	19.5933	128.112263	19.766482	126.214353	0.900748	205.51018209	31.33811175	104.3214	55141.3245949074	2009-11-06 07:47:25	55142.9515277778	2009-11-07 22:50:12	404035010	71.0335	70	71.0335	71.0335	0	71.0335	2	2	0	2	1	0	0	47.461	47.461	140.5559	0	PROCESSED	57549.2155902778	2016-06-10 05:10:27	55532	2010-12-02 00:00:00	55166.2074189815	2009-12-01 04:58:41	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/ver3.0/404035010/	Quick Look
459	WR140	305.2159	43.8446	304.793528	43.684914	327.480092	60.454485	80.96257668	4.11237193	190.1825	54844.5415162037	2009-01-13 12:59:47	54846.500162037	2009-01-15 12:00:14	403030010	89.4068	80	89.4068	89.4068	0	89.4068	2	2	0	2	1	0	0	78.0557	78.0557	169.1969	1	PROCESSED	57545.2609606482	2016-06-06 06:15:47	55328	2010-05-12 00:00:00	54861.8550115741	2009-01-30 20:31:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030157	WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	3	AO3	X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403030010/	Quick Look
460	WR140	305.211	43.8318	304.788544	43.672134	327.46168	60.444795	80.94998516	4.10805919	199.7371	54835.3583449074	2009-01-04 08:36:01	54836.4252199074	2009-01-05 10:12:19	403031010	47.2664	40	47.2664	47.2664	0	47.2824	2	2	0	2	1	0	0	45.303	45.303	92.1618	0	PROCESSED	57545.1036921296	2016-06-06 02:29:19	55328	2010-05-12 00:00:00	54850.2164583333	2009-01-19 05:11:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030157	WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	3	AO3	X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403031010/	Quick Look
461	GX 340+0	251.4463	-45.6133	250.537018	-45.522593	255.990327	-23.069192	339.58535361	-0.07953483	81.21	54892.2765740741	2009-03-02 06:38:16	54894.8168287037	2009-03-04 19:36:14	403060010	107.3127	100	107.3145	107.3127	0	107.3145	2	2	0	2	1	0	0	86.104	86.104	219.4467	1	PROCESSED	57545.7913541667	2016-06-06 18:59:33	55329	2010-05-13 00:00:00	54908.7293055556	2009-03-18 17:30:12	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031164	In this proposal we request to observe accreting neutron stars sources GX 340+0, GX 3+1 and GX 13+1. The observational goal of the observations is to collect high-spectral resolution data in the region of K$_alpha$ iron line. Our scientific motivation is to put the origin of the line emission under additional theoretical scrutiny. We wish to compare the performance of the wind-reprocessing model to relativistic model in as many sources as possible. This proposal is a part of our broader effort to investigate the origin of iron emission line in Galactic X-ray binaries, which includes a parallel proposal to observe WD binaries.	GALACTIC POINT SOURCES	4	B	NIKOLAI SHAPOSHNIKOV		USA	3	AO3	IRON KALPHA EMISSION LINE DIAGNOSTICS IN ACCRETING NEUTRON STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403060010/	Quick Look
462	GK PER	52.8202	43.8404	51.968435	43.670553	61.500851	24.010688	151.00566373	-10.1477205	257.5144	54875.4415277778	2009-02-13 10:35:48	54876.0899884259	2009-02-14 02:09:35	403081010	30.3888	30	30.3888	30.3888	0	30.3888	2	2	0	2	1	0	0	27.3999	27.3999	55.9979	2	PROCESSED	57545.5260648148	2016-06-06 12:37:32	55330	2010-05-14 00:00:00	54893.4257407407	2009-03-03 10:13:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	033107	We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.	GALACTIC POINT SOURCES	4	C	TAKAYUKI YUASA	THOMAS HARRISON	JUS	3	AO3	SURVEY OBSERVATION OF INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403081010/	Quick Look
463	V603 AQL	282.2246	0.5976	281.586541	0.540157	283.33615	23.473967	33.17431822	0.83751501	93.9529	55267.0156597222	2010-03-12 00:22:33	55267.9773032407	2010-03-12 23:27:19	404020010	34.9173	30	34.9309	34.9173	0	34.9309	2	2	0	2	1	0	0	30.2045	30.2045	83.0778	1	PROCESSED	57550.8656018518	2016-06-11 20:46:28	55645	2011-03-25 00:00:00	55279.4471296296	2010-03-24 10:43:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040095	The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail.	GALACTIC POINT SOURCES	4	B	KEI SAITOU		JAP	4	AO4	IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404020010/	Quick Look
464	PQ GEM	117.7967	14.685	117.09108	14.813297	116.98609	-6.189538	206.10344887	19.72488518	295.2889	54933.5737037037	2009-04-12 13:46:08	54934.6329166667	2009-04-13 15:11:24	404030010	46.7387	40	46.7387	46.7387	0	46.7387	2	2	0	2	1	0	0	43.2479	43.2479	91.5079	0	PROCESSED	57546.1405787037	2016-06-07 03:22:26	55324	2010-05-08 00:00:00	54949.5317939815	2009-04-28 12:45:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040113	We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.	GALACTIC POINT SOURCES	4	A	TAKAYUKI YUASA		JAP	4	AO4	SURVEY OBSERVATION OF INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404030010/	Quick Look
465	4U 1608-52	243.1847	-52.3651	242.223789	-52.237385	251.315712	-30.647315	330.96850701	-0.81056533	96.6085	55266.077650463	2010-03-11 01:51:49	55267.0072222222	2010-03-12 00:10:24	404044010	34.0101	30	34.0101	34.0101	0	34.0101	2	2	0	2	1	0	0	30.194	30.194	80.2978	0	PROCESSED	57550.8305902778	2016-06-11 19:56:03	55647	2011-03-27 00:00:00	55279.4591666667	2010-03-24 11:01:12	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/ver3.0/404044010/	Quick Look
466	A 0535+26	84.7291	26.2457	83.952015	26.21825	85.269487	2.891446	181.50526016	-2.67952465	272.2555	55292.5024074074	2010-04-06 12:03:28	55293.7029282407	2010-04-07 16:52:13	404055010	3.1779	45	3.1779	3.4604	0	3.1779	2	2	0	2	1	0	0	34.3928	34.3928	103.7158	1	PROCESSED	57553.0049074074	2016-06-14 00:07:04	55689	2011-05-08 00:00:00	55323.4435532407	2010-05-07 10:38:43	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/ver3.0/404055010/	Quick Look
467	4U 0115+63	19.6209	63.7559	18.795542	63.493074	49.810072	49.806241	125.91670035	1.04099954	84.7167	55747.0027430556	2011-07-05 00:03:57	55748.0529976852	2011-07-06 01:16:19	406048010	24.279	50	24.28	24.279	0	24.2839	2	2	0	2	1	0	0	45.1272	45.1272	90.7279	1	PROCESSED	57602.5201157407	2016-08-02 12:28:58	56163	2012-08-24 00:00:00	55778.4298611111	2011-08-05 10:19:00	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/ver3.0/406048010/	Quick Look
468	CYGNUS X-1	299.5791	35.2719	299.109539	35.135475	313.68862	54.318776	71.39029863	3.11127562	84.0536	54944.1674768518	2009-04-23 04:01:10	54944.6252777778	2009-04-23 15:00:24	404075040	18.014	300	18.0166	18.014	0	18.0166	1	1	0	1	1	0	0	16.3277	16.3277	39.55	0	PROCESSED	57546.2094097222	2016-06-07 05:01:33	54922	2009-04-01 00:00:00	54966.3125	2009-05-15 07:30:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075040/	Quick Look
469	GX 304-1	195.3153	-61.5986	194.542717	-61.329512	225.389902	-49.202492	304.10001953	1.25086712	115.9338	55957.437037037	2012-01-31 10:29:20	55959.1669444444	2012-02-02 04:00:24	406060010	16.5243	65	16.6912	16.5243	0	16.6912	2	2	0	2	1	0	0	58.7124	58.7124	149.4321	3	PROCESSED	57604.5523148148	2016-08-04 13:15:20	56399	2013-04-17 00:00:00	56033.2695023148	2012-04-16 06:28:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061235	We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. 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 II: NEW LINES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406060010/	Quick Look
470	HD162020	267.6612	-40.3294	266.784393	-40.315902	268.126935	-16.903295	350.72995016	-6.73261971	268.3343	55816.4132291667	2011-09-12 09:55:03	55816.727962963	2011-09-12 17:28:16	406037020	15.0362	15	15.0442	15.0442	0	15.0362	2	2	0	2	1	0	0	15.5829	15.5829	27.1839	0	PROCESSED	57603.1194328704	2016-08-03 02:51:59	56218	2012-10-18 00:00:00	55851.4394444444	2011-10-17 10:32:48	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/ver3.0/406037020/	Quick Look
471	HD162020	267.6578	-40.3138	266.781124	-40.300286	268.12395	-16.887741	350.74222411	-6.72254511	106.352	56005.8535069444	2012-03-19 20:29:03	56006.0626157407	2012-03-20 01:30:10	406038010	10.4286	10	10.4373	10.4373	0	10.4286	1	1	0	1	1	0	0	7.673	7.673	18.0559	0	PROCESSED	57604.9610185185	2016-08-04 23:03:52	56435	2013-05-23 00:00:00	56068.625474537	2012-05-21 15:00:41	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/ver3.0/406038010/	Quick Look
472	U GEM IN OUTBURST	118.7732	21.9928	118.033393	22.125213	116.515178	1.161478	199.23241259	23.39259554	281.117	56029.4105324074	2012-04-12 09:51:10	56030.750162037	2012-04-13 18:00:14	407035010	50.2547	50	50.2547	50.2547	0	50.2547	2	2	0	2	1	0	0	47.2967	47.2967	115.7079	1	PROCESSED	57605.2002199074	2016-08-05 04:48:19	56415	2013-05-03 00:00:00	56044.3887731482	2012-04-27 09:19:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070065	It has been believed that the optically thin boundary layer in dwarf novae (DNe) turns into optically thick state in outburst, and, as a result, hard optically thin X-ray emission becomes weaker than in quiescence. This theory was verified in multi-waveband observations of SS Cyg. The DN U Gem, however, does not follow this scenario, and the hard X-ray intensity increases in outburst as well as soft X-ray emission. We propose ToO observations of U Gem both in quiescence and in outburst in order to understand behavior of DNe in X-rays in general, by means of detailed spectroscopy of the soft disk blackbody component, the hard component reflected off the white dwarf, and a 6.4 keV iron line. This study eventually enables us to understand the origin of the Galactic Ridge X-ray Emission.	GALACTIC POINT SOURCES	4	B	TAKAYUKI HAYASHI		JAP	7	AO7-TOO	OBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407035010/	Quick Look
473	HERCULES X-1	254.4605	35.3288	254.009904	35.404408	245.996246	57.479663	58.13264186	37.51848299	268.7999	56189.3538310185	2012-09-19 08:29:31	56190.0300231482	2012-09-20 00:43:14	407051010	25.5356	20	25.5436	25.5494	0	25.5356	2	2	0	2	1	0	0	25.0879	25.0879	58.4219	0	PROCESSED	57607.1017013889	2016-08-07 02:26:27	56590	2013-10-25 00:00:00	56218.5228472222	2012-10-18 12:32:54	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/ver3.0/407051010/	Quick Look
474	1FGL J1018.6-5856	154.7377	-58.9433	154.295067	-58.691919	196.56156	-60.86748	284.35288518	-1.68600623	306.342	56102.9882407407	2012-06-24 23:43:04	56103.3696875	2012-06-25 08:52:21	407070010	17.4473	20	17.4645	17.4633	0	17.4473	2	2	0	2	1	0	0	14.4474	14.4474	32.9499	2	PROCESSED	57606.4834722222	2016-08-06 11:36:12	56480	2013-07-07 00:00:00	56114.1719328704	2012-07-06 04:07:35	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/ver3.0/407070010/	Quick Look
475	LMC X-3	84.7483	-64.0713	84.678356	-64.09698	46.246737	-86.69028	273.56080053	-32.07680965	285.8008	56379.6769444445	2013-03-28 16:14:48	56382.4793634259	2013-03-31 11:30:17	407086010	101.809	100	101.817	101.825	0	101.809	2	2	0	2	1	0	0	92.7246	92.7246	242.1019	1	PROCESSED	57611.0169560185	2016-08-11 00:24:25	56757	2014-04-10 00:00:00	56391.8067592593	2013-04-09 19:21:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072002	We propose a 100 ksec triggered Suzaku observation of the low/hard state of the black hole LMC X-3. This will constrain the disc emission and Fe line profile in this state, both of which are currently very controversial. LMC X-3 has very low interstellar absorption, so gives the best view of the low temperature/low luminosity disc component in this state. Its moderate flux means it can be observed in standard imaging modes without pileup (further enhancing visibility of the disc as these modes are well calibrated down to 0.4 keV) and making the Fe line profile analysis straightforward. Historically LMC X-3 enters a low/hard state on average once a year. Suzaku will be triggered based on an alert from our Swift monitoring program that the source has entered the low/hard state.	GALACTIC POINT SOURCES	4	A	MARI KOLEHMAINEN		EUR	7	AO7-TOO	A TOO OF LMC X-3: IS THE DISC TRUNCATED IN THE LOW/HARD STATE OF BLACK HOLE BINARIES?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407086010/	Quick Look
476	SAGITTARIUS A*	266.4172	-29.0091	265.622479	-28.989771	266.842554	-5.607236	359.94331347	-0.04710749	285.0015	56554.8566087963	2013-09-19 20:33:31	56555.4439930556	2013-09-20 10:39:21	408017030	20.2613	20	20.268	20.2613	0	20.268	2	2	0	2	1	0	0	20.549	20.549	50.7419	1	PROCESSED	57612.6558217593	2016-08-12 15:44:23	56956	2014-10-26 00:00:00	56588.6928935185	2013-10-23 16:37:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017030/	Quick Look
477	V1159 ORI	82.2495	-3.563	81.626179	-3.602056	81.331403	-26.771731	206.52568579	-19.93854352	268.4348	56732.3915856482	2014-03-16 09:23:53	56737.0939583333	2014-03-21 02:15:18	408029010	200.5487	200	200.5567	200.5487	0	200.5567	3	2	0	2	1	0	0	188.9927	188.9927	404.0226	3	PROCESSED	57614.1201967593	2016-08-14 02:53:05	56383	2013-04-01 00:00:00	56807.8867708333	2014-05-30 21:16:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081211	We propose two 200 ks Suzaku observations of the dwarf nova V1159 Ori, chosen as our target because it is a known X-ray source with an extremely short (~4 day) outburst cycle. Each proposed observation will take ~5 calendar days and cover a complete outburst cycle. The dense X-ray coverage of the early rise in particular will be unprecedented for any dwarf nova, which is essential to further our understanding of the response of the boundary layer to the increased mass flux from the Keplerian accretion disk. We will also determine whether X-ray flux increases or decreases during quiescence to test the disk instability model. We will interpret the detailed picture of V1159 Ori in the context of existing, though less complete, X-ray campaigns on several other dwarf novae.	GALACTIC POINT SOURCES	4	A	KOJI MUKAI		USA	8	AO8	X-RAY EMISSION THROUGH COMPLETE OUTBURST CYCLES OF THE DWARF NOVA V1159 ORI	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408029010/	Quick Look
478	SERPENS X-1	279.9926	5.0265	279.375861	4.979658	281.287327	28.076343	36.11096598	4.83541867	266.6732	56566.4312037037	2013-10-01 10:20:56	56570.3821759259	2013-10-05 09:10:20	408033010	1.7605	250	9.5056	34.8553	0	1.7605	2	2	0	2	1	0	0	130.3293	130.3293	341.2899	2	PROCESSED	57612.9481018518	2016-08-12 22:45:16	57198	2015-06-25 00:00:00	56588.8182060185	2013-10-23 19:38:13	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/ver3.0/408033010/	Quick Look
479	SWIFT J1753.5-0127	268.3654	-1.4463	267.717637	-1.436793	268.227765	21.984126	24.9013847	12.1907035	84.8023	56750.7354398148	2014-04-03 17:39:02	56752.4452777778	2014-04-05 10:41:12	409051010	59.7028	50	59.7028	59.7108	0	59.7226	2	2	0	2	1	0	0	53.6812	53.6812	147.7095	2	PROCESSED	57614.197025463	2016-08-14 04:43:43	57157	2015-05-15 00:00:00	56789.6957175926	2014-05-12 16:41:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091243	Due to the presence of a steady jet, constraining the properties of black hole systems in their hard state is important for understanding accretion disks and jets. 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? This proposal includes the use of Suzaku, NuSTAR, and radio observations to address these questions. A main diagnostic of the accretion geometry is the Compton reflection component, and the combination of Suzaku and NuSTAR covers, with very good energy resolution and sensitivity, the iron emission line, the absorption edges, and the hard X-ray reflection hump.	GALACTIC POINT SOURCES	4	A	JOHN TOMSICK		USA	9	AO9-TOO	CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409051010/	Quick Look
480	HD161103	266.1888	-27.2272	265.405227	-27.206791	266.594492	-3.831151	1.35850162	1.05434609	105.2351	54884.7946643518	2009-02-22 19:04:19	54886.7057175926	2009-02-24 16:56:14	403001010	71.5249	60	71.5329	71.5249	0	71.5409	2	2	0	2	1	0	0	59.6647	59.6647	165.0858	1	PROCESSED	57545.6533217593	2016-06-06 15:40:47	55330	2010-05-14 00:00:00	54903.6732523148	2009-03-13 16:09:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030005	We propose Suzaku observations of gamma Cas analogues. The sources in this class are characterized by extremely high thermal temperature and iron fluorescent line. We aim to identify the hard X-ray production site using the XIS's spectral capability at the iron K complex and the wide-band sensitivity combining XIS and HXD PIN.	GALACTIC POINT SOURCES	4	B	JUNICHIRO MIURA		JAP	3	AO3	SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403001010/	Quick Look
481	AQL X-1	287.8171	0.5794	287.178828	0.495683	289.378182	22.829317	35.71359616	-4.14591745	272.6027	54388.3395833333	2007-10-15 08:09:00	54388.7225	2007-10-15 17:20:24	402053040	17.9157	15	17.9157	17.9157	0	17.9157	2	2	0	2	1	0	0	17.6682	17.6682	33.08	0	PROCESSED	57540.2752893518	2016-06-01 06:36:25	54769	2008-10-30 00:00:00	54402.4060648148	2007-10-29 09:44:44	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/ver3.0/402053040/	Quick Look
482	AX J1846.8-0240	281.7182	-2.6613	281.064619	-2.716297	282.480418	20.272966	30.04319345	-0.19850989	89.4057	56018.0125115741	2012-04-01 00:18:01	56019.1146990741	2012-04-02 02:45:10	407019010	37.6209	40	37.6209	41.6127	0	39.2207	2	2	0	2	1	0	0	37.25	37.25	95.2199	0	PROCESSED	57605.0756944445	2016-08-05 01:49:00	56400	2013-04-18 00:00:00	56033.2323032407	2012-04-16 05:34:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070043	Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution.	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	7	AO7	ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407019010/	Quick Look
483	VELA X-1	135.5377	-40.5514	135.064105	-40.353478	157.048654	-53.915556	263.06039339	3.93722667	314.5441	54634.1981134259	2008-06-17 04:45:17	54635.9043287037	2008-06-18 21:42:14	403045010	104.7096	100	104.7234	104.7096	0	104.7154	2	2	0	2	1	0	0	96.0089	96.0089	147.3899	1	PROCESSED	57542.8859375	2016-06-03 21:15:45	55010	2009-06-28 00:00:00	54644.4687847222	2008-06-27 11:15:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031153	We propose to observe the well-known X-ray pulsar Vela X-1 (4U0900-40) using Suzaku in order to test models for the circumstellar environment by measuring teh spectrum and searching for variability in the iron line. The line is expected to exhibit changes in intensity and centroid energy as the X-ray beam sweeps around the wind an illuminates material with varying column density, ionization state, and vleocity. In addition we will study the variability in the cyclotron feature. We will compare our observations with detailed hydrodynamical simulations of the stellar wind and its interaction with the compact object.	GALACTIC POINT SOURCES	4	A	TIMOTHY KALLMAN		USA	3	AO3	SPECTROSCOPY OF VELA X-1 (4U0900-40) AND SEARCHES FOR PULSE PHASE VARIABILITY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403045010/	Quick Look
484	HD130693	222.5749	-24.4173	221.849663	-24.21107	227.410153	-7.711774	334.71293898	31.01917553	104.6337	55580.6525925926	2011-01-19 15:39:44	55581.2384375	2011-01-20 05:43:21	405031010	21.3145	20	21.3145	21.3145	0	21.3145	2	2	0	2	1	0	0	17.4625	17.4625	50.6059	2	PROCESSED	57600.6648842593	2016-07-31 15:57:26	55965	2012-02-08 00:00:00	55598.9831597222	2011-02-06 23:35:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050116	Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	5	AO5	QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405031010/	Quick Look
485	AQL X-1	287.8271	0.5745	287.188805	0.490736	289.388235	22.823139	35.71381986	-4.15705073	244.5264	55852.1545486111	2011-10-18 03:42:33	55853.110625	2011-10-19 02:39:18	406010010	9.4948	40	9.5968	9.4948	0	9.5968	2	1	0	1	1	0	0	35.325	35.325	82.5878	1	PROCESSED	57603.4610763889	2016-08-03 11:03:57	56240	2012-11-09 00:00:00	55873.1222337963	2011-11-08 02:56:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060036	We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object.	GALACTIC POINT SOURCES	4	A	KAZUTAKA YAMAOKA		JAP	6	AO6-TOO	SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406010010/	Quick Look
486	1E1724-3045	261.8859	-30.8016	261.081118	-30.76036	262.965781	-7.558159	356.31902476	2.29998715	95.7568	57113.6866087963	2015-04-01 16:28:43	57115.0028935185	2015-04-03 00:04:10	409024010	60.2315	60	60.2315	60.2515	0	60.2337	3	3	0	3	0	0	0	0	0	0	0	PROCESSED	57617.9445833333	2016-08-17 22:40:12	57493	2016-04-15 00:00:00	57126.4247106482	2015-04-14 10:11:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090106	Low Mass X-ray Binaries(LMXBs) have soft and hard state. After breakthrough of hard state accretion geometry in LMXBs Sakurai et al.2012,2013), we found a clue to connect hard/soft states. first, we found that the geometry of GS1826-238 is similar to that of soft state, and is understood in the framework of Sakurai et al. (2012,2013). Second, we found a surprising relation between two physical quantities of corona, which roughly shows a continuous change of relation between soft/hard states in contrast with a dramatic change of their spectra. In order to confirm such a continuous relation between two distinct states, we propose a LMXB, which usually shows hard state with high luminosity.	GALACTIC POINT SOURCES	4	B	KO ONO		JAP	9	AO9	TOWARD COMPREHENSIVE UNDERSTANDING OF LMXBS ~OBSERVATION OF HARD STATE WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409024010/	Quick Look
487	XB 1916-053	289.7027	-5.2415	289.037629	-5.333849	290.520863	16.806325	31.35614078	-8.46800846	250.2538	54047.242974537	2006-11-08 05:49:53	54048.1119791667	2006-11-09 02:41:15	401095010	38.4647	40	39.0967	39.0887	38.4647	39.0967	2	2	2	2	1	0	0	37.4857	37.4857	75.082	2	PROCESSED	57536.0684259259	2016-05-28 01:38:32	54735	2008-09-26 00:00:00	54088.866087963	2006-12-19 20:47:10	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012038	We propose Suzaku observations of the dipping low mass X-ray binaries XB1916-053, XB1323-619, EXO0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been recently demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the photoionised absorbers and reliably determine the values of the ionization parameter for each source, and the simultaneous spectra of HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components and to extend the photoionized absorber fits to higher energies. This will test the validity of the ionized absorber model also >10 keV.	GALACTIC POINT SOURCES	4	A	MARIA DIAZ TRIGO		EUR	1	AO1	BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401095010/	Quick Look
488	HD432	2.3079	59.1397	1.651195	58.861536	35.116502	51.20601	117.53319828	-3.2889222	246.0535	54471.6956944444	2008-01-06 16:41:48	54472.297349537	2008-01-07 07:08:11	402034020	26.9844	27	26.9844	26.9844	0	26.9844	1	1	0	1	1	0	0	24.601	24.601	51.9759	0	PROCESSED	57541.2823958333	2016-06-02 06:46:39	54871	2009-02-09 00:00:00	54483.3863773148	2008-01-18 09:16:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021016	Suzaku XIS spectra of three "X-ray deficient" Hertzsprung gap giants will explore why they display anomalous coronal behavior compared with cooler giants only slightly further advanced in their evolution. The apparent sharp transition in coronal properties on the way to helium flash might be caused by disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. A key discriminator is the coronal energy distribution, especially enhanced and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution; all three have supporting high resolution UV spectra. Expanding the sample of high quality, high energy information on this key class of objects is essential for probing their odd behavior.	GALACTIC POINT SOURCES	4	C	THOMAS AYRES		USA	2	AO2	ANOMALOUS CORONAE OF HERTZSPRUNG GAP GIANTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402034020/	Quick Look
489	1RXS J062518.2+73343	96.3307	73.5671	94.750009	73.593987	92.79758	50.188181	140.86801575	24.12512545	262.0383	54570.0388310185	2008-04-14 00:55:55	54571.1252777778	2008-04-15 03:00:24	403004010	50.3267	50	50.3267	50.3267	0	50.3267	2	2	0	2	1	0	0	50.1253	50.1253	93.8488	0	PROCESSED	57542.3202430556	2016-06-03 07:41:09	54953	2009-05-02 00:00:00	54581.2328472222	2008-04-25 05:35:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030009	Soft Intermediate Polar (IP) is a group of IPs whose X-ray spectra are extremely soft compared with general IPs. Recent observations reveal that some soft IPs have a soft blackbody emission component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand comprehensively the emission characteristics of polars and IPs in the soft X-ray band, and to follow possible evolutionary link from IPs to polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure its temperature and flux systematically.	GALACTIC POINT SOURCES	4	B	MANABU ISHIDA		JAP	3	AO3	OBSERVATIONS OF SOFT INTERMEDIATE POLARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403004010/	Quick Look
490	MARS-P17	103.5439	25.0908	102.776216	25.154177	102.256232	2.224275	190.5741012	11.71183533	298.237	54560.6601041667	2008-04-04 15:50:33	54560.743287037	2008-04-04 17:50:20	403006170	1.9782	100	1.9782	1.9782	0	1.9782	1	1	0	1	1	0	0	1.9596	1.9596	7.182	0	PROCESSED	57542.0674074074	2016-06-03 01:37:04	54953	2009-05-02 00:00:00	54578.0406597222	2008-04-22 00:58:33	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006170/	Quick Look
491	4U 1820-30	275.9205	-30.4212	275.116914	-30.447977	275.132756	-7.085901	2.7347979	-7.94197311	270.4164	55124.2356134259	2009-10-20 05:39:17	55124.7925810185	2009-10-20 19:01:19	404069070	24.0566	100	24.0567	24.0726	0	24.0566	3	1	0	2	1	0	0	18.9035	18.9035	48.1079	0	PROCESSED	57548.9193981482	2016-06-09 22:03:56	55503	2010-11-03 00:00:00	55134.2427314815	2009-10-30 05:49:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069070/	Quick Look
492	CYGNUS X-1	299.5434	35.2592	299.073819	35.122926	313.634234	54.316619	71.36423878	3.12954641	57.7977	54971.0242592593	2009-05-20 00:34:56	54971.6043865741	2009-05-20 14:30:19	404075080	21.3404	300	21.3404	21.3484	0	21.3404	2	1	0	2	1	0	0	17.4954	17.4954	50.1199	1	PROCESSED	57546.6088888889	2016-06-07 14:36:48	54922	2009-04-01 00:00:00	54992.6546875	2009-06-10 15:42:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075080/	Quick Look
493	HER X-1	254.4936	35.2712	254.042629	35.346654	246.066668	57.428555	58.06646448	37.48255114	250.0637	55467.7830208333	2010-09-28 18:47:33	55468.2362962963	2010-09-29 05:40:16	405058010	21.3567	20	21.3567	21.3567	0	21.5034	2	2	0	1	1	0	0	18.9323	18.9323	39.1599	0	PROCESSED	57553.5804050926	2016-06-14 13:55:47	55843	2011-10-09 00:00:00	55477.2237152778	2010-10-08 05:22:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052001	We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity?	GALACTIC POINT SOURCES	4	B	R DIGER STAUBERT		EUR	5	AO5	VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405058010/	Quick Look
494	HD162020	267.6611	-40.3282	266.784303	-40.314701	268.126834	-16.902096	350.73095661	-6.73195128	265.867	55808.0919560185	2011-09-04 02:12:25	55808.4078703704	2011-09-04 09:47:20	406037010	15.9229	15	15.9229	15.9229	0	15.9229	1	1	0	1	1	0	0	15.9406	15.9406	27.2879	2	PROCESSED	57603.0570949074	2016-08-03 01:22:13	56232	2012-11-01 00:00:00	55865.1159953704	2011-10-31 02:47:02	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/ver3.0/406037010/	Quick Look
495	ETA CARINAE	161.2639	-59.6881	160.777388	-59.424763	202.155739	-58.924842	287.59810122	-0.63296206	310.0122	55766.0329398148	2011-07-24 00:47:26	55766.9286226852	2011-07-24 22:17:13	406039010	42.0302	50	42.0302	42.0302	0	42.0302	1	1	0	1	1	0	0	49.0937	49.0937	77.3839	0	PROCESSED	57602.6625462963	2016-08-02 15:54:04	56163	2012-08-24 00:00:00	55785.0281712963	2011-08-12 00:40:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061205	Eta Car is the nearest highly unstable extremely massive star and a key object for understanding how mass and angular momentum change as an extremely massive star heads towards hypernova. Periodic minima in X-rays and other wavebands show it as an extremely eccentric binary with a massive companion. A surprising change in the X-ray emission during the January 2009 X-ray minimum probably indicates a large-scale variation in the LBV primary's mass loss rate. We propose a Suzaku observation in AO6 to monitor the change of the absorption column in the line of sight and the non-thermal emission above 10 keV. The observation will help to study geometry of the binary orbit of Eta Car and the mechanism of the non-thermal emission.	GALACTIC POINT SOURCES	4	B	KENJI HAMAGUCHI		USA	6	AO6	MONITORING DYNAMICAL MASS LOSS FROM ETA CAR WITH SUZAKU: APASTRON	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406039010/	Quick Look
496	EK TRA	228.5098	-65.0893	227.42561	-64.902826	246.763957	-44.956932	317.22984637	-6.25468419	278.6002	56149.7387152778	2012-08-10 17:43:45	56150.8473611111	2012-08-11 20:20:12	407044010	77.8344	70	77.8504	77.8344	0	77.8504	2	2	0	2	1	0	0	69.8973	69.8973	95.7779	2	PROCESSED	57606.8494907407	2016-08-06 20:23:16	56540	2013-09-05 00:00:00	56170.0360532407	2012-08-31 00:51:55	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/ver3.0/407044010/	Quick Look
497	1RXSJ194246.3+103339	295.6976	10.5399	295.103359	10.420476	299.93501	31.348954	48.24168916	-6.37340779	280.0002	55848.1433564815	2011-10-14 03:26:26	55848.635625	2011-10-14 15:15:18	406035010	20.4889	20	20.4889	20.4889	0	20.4889	3	2	0	2	1	0	0	17.142	17.142	42.508	0	PROCESSED	57603.4189583333	2016-08-03 10:03:18	56240	2012-11-09 00:00:00	55873.0004861111	2011-11-08 00:00:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060097	We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray.	GALACTIC POINT SOURCES	4	B	HIROMITSU TAKAHASHI		JAP	6	AO6	SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406035010/	Quick Look
498	SXDB2	305.4808	37.2375	305.012336	37.076849	322.528101	54.400691	75.63404607	0.19419319	72.9993	57170.7872453704	2015-05-28 18:53:38	57171.5090972222	2015-05-29 12:13:06	410014010	29.3922	30	29.3959	29.3947	0	29.3922	3	3	0	3	0	0	0	0	0	0	0	PROCESSED	57618.772650463	2016-08-18 18:32:37	57558	2016-06-19 00:00:00	57190.4609259259	2015-06-17 11:03:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	100037	The soft X-ray sky below 1 keV is spatially smooth after subtracting the local extended emission structures although the interstellar X-ray absorption column density is high enough to block the extragalactic X-ray photons below 1 keV totally in the Galactic disk. Suzaku reveals the existence of "excess" emissions in the Galactic disk and our observations will allow us to study a spatial distribution of the emissions and constrain the origin.	GALACTIC POINT SOURCES	4	C	IKUYUKI MITSUISHI		JAP	10	AO10	EXPLORING THE ORIGIN OF SOFT X-RAY DIFFUSE BACKGROUND IN THE GALACTIC DISK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410014010/	Quick Look
499	LMC X -3	84.7048	-64.0785	84.635001	-64.10439	45.912813	-86.683865	273.57060216	-32.09537201	185.5067	54822.3015856482	2008-12-22 07:14:17	54823.8675694444	2008-12-23 20:49:18	403020010	73.9738	60	73.9738	73.9818	0	73.9875	2	2	0	2	1	0	0	70.0505	70.0505	135.2838	1	PROCESSED	57545.0347800926	2016-06-06 00:50:05	55206	2010-01-10 00:00:00	54840.5013310185	2009-01-09 12:01:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030102	Ionized iron K absorption lines are commonly observed from high state black hole binaries. Thus the highly ionized plasma are thought to be generally associated with optically thick accretion disks. Huge outflow by the plasma has been confirmed by some of these objects, and thus such plasma is thought to have an important role on accretion flow. In order to establish generality of the plasma by detecting the absorption lines, and to distinguish whether creation mechanism of the plasma is determined by X-ray luminosity or there is another key parameter, we propose Suzaku observation of luminous persistent black hole binary LMC X-3, with exposure of 60ks. This observation will enable us to find critical parameters which determine the creation of the accretion disk wind.	GALACTIC POINT SOURCES	4	C	AYA KUBOTA		JAP	3	AO3	SEARCH FOR IRON K ABSORPTION LINES FROM LMC X-3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403020010/	Quick Look
500	V2129 OPH	246.9149	-24.3651	246.158782	-24.254235	249.041959	-2.587504	353.29078542	16.72506486	88.3342	54866.0202430556	2009-02-04 00:29:09	54866.5821296296	2009-02-04 13:58:16	403074010	21.0335	20	21.0335	21.0335	0	21.0335	2	2	0	2	1	0	0	16.5331	16.5331	48.5339	0	PROCESSED	57545.4470833333	2016-06-06 10:43:48	55329	2010-05-13 00:00:00	54880.5317708333	2009-02-18 12:45:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032022	We propose to observe the classical T Tauri stars CS Cha, MN Lup, V2129 Oph and XZ Tau with the Suzaku XIS to investigate accretion induced X-ray emission in CTTS as evidenced by the presence of excess emission in the soft X-ray regime. Specifically we intend to utilize Suzaku's sensitivity, low background and the capability of the XIS to resolve the OVIII Ly-alpha line from the OVII triplet. XMM-Newton and Chandra grating spectra provide strong evidence for the presence of accretion induced X-ray emission in CTTS, however, due to low SNR and the presence of absorption an accretion scenario often cannot be probed within reasonable exposure times. With the proposed observations we want to investigate a sample of these CTTS showing additional exceptional properties.	GALACTIC POINT SOURCES	4	B	JAN ROBRADE		EUR	3	AO3	ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403074010/	Quick Look
501	SKY(270, +25)	270.2558	25.1504	269.745742	25.150381	270.337589	48.59021	50.99920401	21.68976417	70.6538	55284.5620023148	2010-03-29 13:29:17	55285.2994791667	2010-03-30 07:11:15	404041010	1.7019	25	1.9266	2.0944	0	1.7019	2	2	0	2	1	0	0	5.6211	5.6211	63.7139	1	PROCESSED	57551.0540277778	2016-06-12 01:17:48	55284	2010-03-29 00:00:00	55301.2652314815	2010-04-15 06:21:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041222	Suzaku has recently revealed relativistically broadened Fe Kalpha emission lines in the spectra of neutron star low-mass X-ray binaries (LMXBs). We have now seen these lines in 10 neutron star LMXBs that we have examined, allowing measurements of the inner accretion disk radius, and hence an upper limit on the neutron star radius in all these objects. Only with the sensitivity of Suzaku, its high effective area in the Fe K band, and its broad bandpass has it been possible to robustly determine the shape of the lines. With a longer-term aim of completing a census of iron lines in neutron star LMXBs, we request a total of 200 ks to observe 5 neutron star low-mass X-ray binaries to study the relativistic broadening in the Fe Kalpha emission line profiles.	GALACTIC POINT SOURCES	4	C	EDWARD CACKETT		USA	4	AO4	AN FE KALPHA EMISSION LINE SURVEY OF NEUTRON STAR LMXBS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404041010/	Quick Look
502	4U 1210-64	183.3036	-64.8719	182.632422	-64.593786	222.057216	-55.171704	298.88624165	-2.30082607	98.4956	55553.1591550926	2010-12-23 03:49:11	55555.1488194444	2010-12-25 03:34:18	405045010	79.3476	80	79.3476	79.3476	0	79.3561	2	2	0	2	1	0	0	70.7512	70.7512	171.8799	0	PROCESSED	57554.5554398148	2016-06-15 13:19:50	55961	2012-02-04 00:00:00	55595.085474537	2011-02-03 02:03:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051236	4U 1210-64 is a high mass X-ray binary with a stable 6.7 day period when the long-term (RXTE ASM) light curve is analyzed. However, we observed strong aperiodic variability in a series of pointed observations with the RXTE PCA, to the point of masking this 6.7 day period. Moreover, we have not detected a spin period, even though the accretor is most likely a neutron star. The strong variability is suggestive of accretion from a clumpy wind. We propose a 2-day Suzaku observation of this object (1) to search for unequivocal evidence for a neutron star, such as the spin period and cyclotron features; and (2) to measure the spectral shapes at different flux levels, to investigate the cause of the strong aperiodic variability.	GALACTIC POINT SOURCES	4	C	KOJI MUKAI		USA	5	AO5	4U 1210-64: A HIGHLY VARIABLE X-RAY BINARY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405045010/	Quick Look
503	4U 1957+11	299.8426	11.72	299.251782	11.582704	304.891281	31.61725	51.31417386	-9.31797438	71.6227	55320.4377777778	2010-05-04 10:30:24	55321.4168055556	2010-05-05 10:00:12	405057010	35.796	35	35.804	35.804	0	35.796	2	2	0	2	1	0	0	30.8692	30.8692	84.58	0	PROCESSED	57551.4086226852	2016-06-12 09:48:25	55741	2011-06-29 00:00:00	55375.7567013889	2010-06-28 18:09:39	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/ver3.0/405057010/	Quick Look

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