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 766

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	COMET_8P_TUTTLE-P2_08	40.0642	-36.6693	39.55682	-36.883219	21.03457	-48.879704	242.2833952	-65.12116443	253.2206	54490.9649421296	2008-01-25 23:09:31	54491.0959953704	2008-01-26 02:18:14	502063080	3.5416	4	3.5496	3.5416	0	3.5576	2	2	0	2	1	0	0	3.564	3.564	11.3119	0	PROCESSED	57541.3990509259	2016-06-02 09:34:38	54912	2009-03-22 00:00:00	54546.1411689815	2008-03-21 03:23:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063080/	Quick Look
2	GC_SOUTH_1	268.0988	-29.4771	267.30082	-29.465922	268.32614	-6.047082	0.29758282	-1.54591478	274.6002	56190.0385069444	2012-09-20 00:55:27	56191.3341435185	2012-09-21 08:01:10	507028010	51.7619	50	51.7619	51.7699	0	51.7699	3	3	0	3	1	0	0	41.1534	41.1534	111.9318	1	PROCESSED	57607.1304398148	2016-08-07 03:07:50	56584	2013-10-19 00:00:00	56218.5464930556	2012-10-18 13:06:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070042	We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation.	GALACTIC DIFFUSE EMISSION	5	A	SHINYA NAKASHIMA		JAP	7	AO7	OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507028010/	Quick Look
3	JUPITER	104.4639	23.0622	103.708176	23.129949	103.287865	0.285992	192.81439153	11.62759441	264.6138	56767.1149421296	2014-04-20 02:45:31	56767.448125	2014-04-20 10:45:18	508023110	16.7417	160	16.7417	16.7737	0	16.7657	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57614.9630671296	2016-08-14 23:06:49	57212	2015-07-09 00:00:00	56789.801712963	2014-05-12 19:14:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023110/	Quick Look
4	CYGNUS LOOP BLOWOUT3	312.3799	29.0257	311.853293	28.839005	325.853846	44.599011	72.47923846	-9.33489782	78.1517	55688.6493981482	2011-05-07 15:35:08	55689.9654976852	2011-05-08 23:10:19	506013010	60.2669	60	60.2669	60.2749	0	60.2669	2	2	0	2	1	0	0	55.9803	55.9803	113.6288	1	PROCESSED	57601.9873611111	2016-08-01 23:41:48	56066	2012-05-19 00:00:00	55700.4602083333	2011-05-19 11:02:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060053	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	6	AO6	MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506013010/	Quick Look
5	G54.1+0.3	292.6593	18.8091	292.105949	18.703083	298.434306	40.039537	54.05763723	0.20765467	245.096	54403.6644560185	2007-10-30 15:56:49	54406.3335532407	2007-11-02 08:00:19	502077010	101.6411	100	101.6411	101.6491	0	101.6491	2	2	0	2	1	0	0	92.9235	92.9235	230.5857	3	PROCESSED	57540.4530324074	2016-06-01 10:52:22	54786	2008-11-16 00:00:00	54417.8870833333	2007-11-13 21:17:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022032	A proprietary XMM-Newton observation reveals that the pulsar wind nebula G54.1+0.3 has a very hard spectrum (gamma ~ 1.5) and possibly a break between 5 and 10 keV. We propose a 100 ks SUZAKU observation to confirm unambiguously the presence of the break. If confirmed, the break would pose stringent constraints on models of electron emission and propagation in pulsar wind nebulae.	GALACTIC DIFFUSE EMISSION	5	C	FABRIZIO BOCCHINO		EUR	2	AO2	THE BREAK IN THE HARD X-RAY ENERGY OF THE PULSAR WIND NEBULA G54.1+0.3	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502077010/	Quick Look
6	TYCHO SNR HXD BKGD	9.2173	64.3076	8.488109	64.032592	44.61366	53.051862	121.35322514	1.48051733	84.2005	53915.6541782407	2006-06-29 15:42:01	53916.7606944444	2006-06-30 18:15:24	500025010	51.0088	50	51.0088	51.0088	51.0088	51.0088	2	2	2	2	1	0	0	48.7224	48.7224	95.5939	2	PROCESSED	57534.8010300926	2016-05-26 19:13:29	54302	2007-07-21 00:00:00	54052.5940509259	2006-11-13 14:15:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001099	We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		JAP	0	SWG	SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500025010/	Quick Look
7	GC20	265.6604	-28.73	264.867608	-28.707008	266.169302	-5.346539	359.83402449	0.66365416	262.9349	54385.4117939815	2007-10-12 09:52:59	54385.9099421296	2007-10-12 21:50:19	502008010	23.7786	20	23.7906	23.7866	0	23.7786	2	2	0	2	1	0	0	22.9234	22.9234	43.032	0	PROCESSED	57540.2572337963	2016-06-01 06:10:25	54771	2008-11-01 00:00:00	54403.0227314815	2007-10-30 00:32:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502008010/	Quick Look
8	ASO0376	263.1417	-31.5448	262.331507	-31.509592	264.088273	-8.244108	356.29011362	0.99386623	267.5095	55082.1506365741	2009-09-08 03:36:55	55083.1084606482	2009-09-09 02:36:11	504049010	37.2278	20	38.9878	39.2598	0	37.2278	5	4	0	4	1	0	0	31.8134	31.8134	82.7299	1	PROCESSED	57548.4976041667	2016-06-09 11:56:33	55479	2010-10-10 00:00:00	55113.2260069444	2009-10-09 05:25:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 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 DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504049010/	Quick Look
9	VELA JR P26	132.8787	-46.6693	132.45444	-46.480585	159.781455	-60.154541	266.46476457	-1.49839932	347.0019	54653.4341203704	2008-07-06 10:25:08	54653.837025463	2008-07-06 20:05:19	503038010	14.553	10	14.553	14.553	0	14.553	1	1	0	1	1	0	0	10.9536	10.9536	34.7839	0	PROCESSED	57542.9869675926	2016-06-03 23:41:14	55048	2009-08-05 00:00:00	54679.3709606482	2008-08-01 08:54:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503038010/	Quick Look
10	CYGNUS_LOOP_P8	313.9965	31.4722	313.478406	31.279742	329.042886	46.311836	75.29540263	-8.88432445	62.5181	53868.0059837963	2006-05-13 00:08:37	53868.1717476852	2006-05-13 04:07:19	501028010	4.8706	6	4.8706	4.8706	4.8706	4.8706	2	2	2	2	1	0	0	2.328	2.328	14.316	0	PROCESSED	57534.2851736111	2016-05-26 06:50:39	54394	2007-10-21 00:00:00	53914.3326157407	2006-06-28 07:58:58	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501028010/	Quick Look
11	NEP #4	270.0449	66.5788	270.046703	66.578557	56.874538	89.977746	96.40481628	29.79358389	165.3654	55193.4146875	2009-12-28 09:57:09	55194.4579166667	2009-12-29 10:59:24	504076010	49.8491	50	49.8571	49.8571	0	49.8491	2	2	0	2	1	0	0	43.5039	43.5039	90.114	0	PROCESSED	57550.0085648148	2016-06-11 00:12:20	54922	2009-04-01 00:00:00	55246.2930787037	2010-02-19 07:02:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041101	We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe.	GALACTIC DIFFUSE EMISSION	5	A	STEVEN SNOWDEN		USA	4	AO4	OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504076010/	Quick Look
12	MRK 421 OFFSET	165.3836	38.6302	164.685253	38.899103	150.412438	29.624722	179.31913311	64.35556561	121.9647	55146.4480092593	2009-11-11 10:45:08	55148.3176388889	2009-11-13 07:37:24	504087010	86.0144	75	86.0144	86.0144	0	86.0144	2	2	0	2	1	0	0	64.8804	64.8804	161.5199	3	PROCESSED	57549.3389583333	2016-06-10 08:08:06	55531	2010-12-01 00:00:00	55160.2701041667	2009-11-25 06:28:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041324	The OVII, OVIII, and NeIX absorption lines at z~0 have been discovered in the Chandra/XMM spectra of several bright AGNs, but the location of these absorptions has been debated since their discoveries. Here we request Suzaku observations of the soft X-ray background emission in the vicinity of Mrk 421, to conduct a joint analysis of the emission data with the extensive Chandra absorption data. This analysis will naturally yield an effective length of the absorbing/emitting gas. We have performed pilot studies and obtained a scale length of several kpc for the hot absorbing/emitting gas toward LMC X-3 and Mrk 421. The requested Suzaku observations are particular important to check these results and to further test the models we have developed in our study.	GALACTIC DIFFUSE EMISSION	5	B	YANGSEN YAO		USA	4	AO4	A JOINT X-RAY ABSORPTION AND EMISSION STUDY OF THE HOT GAS TOWARD MRK 421	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504087010/	Quick Look
13	GALACTIC_BULGE10	268.297	-31.6627	267.484676	-31.652449	268.525852	-8.230314	358.49964198	-2.80216044	277.1297	55091.579525463	2009-09-17 13:54:31	55093.1508564815	2009-09-19 03:37:14	504093010	53.2416	50	53.2495	53.2416	0	53.2575	2	2	0	2	1	0	0	46.9072	46.9072	135.734	1	PROCESSED	57548.6254513889	2016-06-09 15:00:39	54922	2009-04-01 00:00:00	55110.3193865741	2009-10-06 07:39:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504093010/	Quick Look
14	GALACTIC_BULGE8	267.0897	-31.0498	266.281644	-31.033699	267.475091	-7.634163	358.49976827	-1.60277837	260.4349	55088.8177777778	2009-09-14 19:37:36	55090.3043287037	2009-09-16 07:18:14	504091010	51.3316	50	51.3316	51.3392	0	51.3316	2	2	0	2	1	0	0	47.7514	47.7514	128.4258	2	PROCESSED	57548.5976041667	2016-06-09 14:20:33	54922	2009-04-01 00:00:00	55109.4226736111	2009-10-05 10:08:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504091010/	Quick Look
15	VELA PWN N4	128.8415	-44.0453	128.410682	-43.871484	152.26227	-59.375821	262.64764922	-2.10667439	326.4998	56110.0169097222	2012-07-02 00:24:21	56110.3459953704	2012-07-02 08:18:14	507051010	17.289	15	17.289	17.289	0	17.289	2	2	0	2	1	0	0	17.6558	17.6558	28.4019	0	PROCESSED	57606.5331018518	2016-08-06 12:47:40	56646	2013-12-20 00:00:00	56280.6029050926	2012-12-19 14:28:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070103	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	7	AO7	HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507051010/	Quick Look
16	VELA PWN W1	128.3503	-45.1912	127.929525	-45.019236	152.791152	-60.544208	263.35940671	-3.07091685	303.5014	56438.6169444444	2013-05-26 14:48:24	56439.0342476852	2013-05-27 00:49:19	508042010	14.1172	15	14.1172	14.1252	0	14.1252	1	1	0	1	1	0	0	13.2844	13.2844	36.0239	0	PROCESSED	57611.3765046296	2016-08-11 09:02:10	56864	2014-07-26 00:00:00	56498.6138888889	2013-07-25 14:44:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080090	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered.	GALACTIC DIFFUSE EMISSION	5	B	KOJI MORI		JAP	8	AO8	SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508042010/	Quick Look
17	G359.0-0.9 NW	266.56	-30.3287	265.756777	-30.310042	266.999862	-6.92337	358.88098313	-0.83974756	102	56723.5510648148	2014-03-07 13:13:32	56724.8162268518	2014-03-08 19:35:22	508058010	52.0885	50	52.0885	52.0965	0	52.1045	2	2	0	2	1	0	0	45.5738	45.5738	109.2758	2	PROCESSED	57613.9935416667	2016-08-13 23:50:42	57100	2015-03-19 00:00:00	56734.6649189815	2014-03-18 15:57:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080113	We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	8	AO8	FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508058010/	Quick Look
18	SS433_JET_KNOT	288.5694	4.9037	287.951117	4.816458	290.852472	27.010013	39.90628699	-2.82264549	256.6998	56597.9130555556	2013-11-01 21:54:48	56600.2502314815	2013-11-04 06:00:20	508024010	106.8942	100	106.8942	106.8942	0	106.8942	2	2	0	2	1	0	0	102.4583	102.4583	201.8897	3	PROCESSED	57613.2427777778	2016-08-13 05:49:36	56980	2014-11-19 00:00:00	56611.6875578704	2013-11-15 16:30:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080065	We propose an observation of the jet of SS 433. Our purpose is to detect high-temperature diffuse plasma component made by the black hole jet.	GALACTIC DIFFUSE EMISSION	5	C	HIDEKI UCHIYAMA		JAP	8	AO8	SEARCHING DIFFUSE HOT-PLASMA COMPONENT MADE BY A BLACK HOLE JET OF SS 433	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508024010/	Quick Look
19	GC_SGR_B_EAST	267.0203	-28.3518	266.229607	-28.335406	267.358668	-4.938031	0.77973231	-0.1584432	71.8708	54162.5141203704	2007-03-03 12:20:20	54164.5273726852	2007-03-05 12:39:25	501039010	96.4018	100	96.4018	96.4018	0	96.4018	2	2	0	2	1	0	0	91.0829	91.0829	173.9318	3	PROCESSED	57537.6522800926	2016-05-29 15:39:17	54736	2008-09-27 00:00:00	54171.4429050926	2007-03-12 10:37:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010060	We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	1	AO1	OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501039010/	Quick Look
20	COMET_8P_TUTTLE-P1-5	28.1493	7.0036	27.492979	6.757378	28.646774	-4.267305	148.58110255	-52.79544349	248.5006	54470.7825810185	2008-01-05 18:46:55	54470.8487384259	2008-01-05 20:22:11	502062050	1.6746	2	1.6746	1.6746	0	1.6746	1	1	0	1	1	0	0	1.703	1.703	5.6861	0	PROCESSED	57540.9980208333	2016-06-01 23:57:09	54908	2009-03-18 00:00:00	54542.2043055556	2008-03-17 04:54:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062050/	Quick Look
21	COMET_8P_TUTTLE-P2_13	40.3641	-37.3366	39.860845	-37.549577	20.8839	-49.581867	243.65335896	-64.71445889	253.6857	54491.6297106482	2008-01-26 15:06:47	54491.762662037	2008-01-26 18:18:14	502063130	6.5907	6.7	6.6147	6.5987	0	6.5907	1	1	0	1	1	0	0	5.0221	5.0221	11.4799	0	PROCESSED	57541.4103356482	2016-06-02 09:50:53	54912	2009-03-22 00:00:00	54546.2204861111	2008-03-21 05:17:30	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063130/	Quick Look
22	HESSJ1741-A	265.3548	-30.1316	264.55314	-30.107106	265.945938	-6.755753	358.50289854	0.15030933	73.8229	54886.7117013889	2009-02-24 17:04:51	54888.0419328704	2009-02-26 01:00:23	503076010	52.9323	50	52.9323	52.9323	0	52.9323	2	2	0	2	1	0	0	43.7708	43.7708	114.9158	1	PROCESSED	57545.6752546296	2016-06-06 16:12:22	55330	2010-05-14 00:00:00	54902.4869791667	2009-03-12 11:41:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030113	HESSJ1741-302 is one of the most darkest TeV unidentified objects which was discovered with the H.E.S.S. telescope recently. The location strongly suggests that the object is physically connected to the diffuse TeV gamma-ray emission along the Galactic plane. On the other hand, there is a pulsar near the object, and it may be an off-set pulsar wind nebula. To clarify the origin of the object, we propose to the observation of HESSJ1741.	GALACTIC DIFFUSE EMISSION	5	C	HIRONORI MATSUMOTO		JAP	3	AO3	DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503076010/	Quick Look
23	BULGE 2	270.6176	-29.5847	269.818763	-29.585758	270.530563	-6.144879	1.30042786	-3.49803376	83.2679	53801.7493981482	2006-03-07 17:59:08	53802.0689699074	2006-03-08 01:39:19	500002010	13.028	10	13.052	13.044	13.036	13.028	1	1	1	1	1	0	0	10.6741	10.6741	27.5999	1	PROCESSED	57533.1394444444	2016-05-25 03:20:48	54247	2007-05-27 00:00:00	54041.664525463	2006-11-02 15:56:55	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001014	Leading .	GALACTIC DIFFUSE EMISSION	5	A	DAN MCCAMMON		JAP	0	SWG	THE SOFT GALACTIC BULGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500002010/	Quick Look
24	DRACO HVC REGION B	243.9603	59.1738	243.739297	59.296448	199.753416	76.165002	90.07720195	42.68363475	80.282	53816.0059953704	2006-03-22 00:08:38	53817.4148611111	2006-03-23 09:57:24	501005010	61.632	60	61.6447	61.644	61.632	61.636	2	2	2	2	1	0	0	60.6865	60.6865	121.7099	2	PROCESSED	57533.3166319444	2016-05-25 07:35:57	54400	2007-10-27 00:00:00	53906.4964583333	2006-06-20 11:54:54	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010069	High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	1	AO1	SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE -	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501005010/	Quick Look
25	CYGNUS_LOOP_P9	311.8173	30.594	311.299257	30.409327	326.059392	46.235255	73.41991066	-7.98099126	239.9998	54416.7228935185	2007-11-12 17:20:58	54417.2502199074	2007-11-13 06:00:19	501019010	19.5656	15	19.5656	19.5656	0	19.5656	2	2	0	2	1	0	0	17.3446	17.3446	45.5379	0	PROCESSED	57540.4965393518	2016-06-01 11:55:01	54798	2008-11-28 00:00:00	54430.2327546296	2007-11-26 05:35:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501019010/	Quick Look
26	COMET_8P_TUTTLE-P2_16	40.5411	-37.7213	40.040278	-37.933718	20.796624	-49.987507	244.42429467	-64.47300408	253.9693	54492.0297106482	2008-01-27 00:42:47	54492.162662037	2008-01-27 03:54:14	502063160	3.7705	4	3.7705	3.7705	0	3.7705	1	1	0	1	1	0	0	3.9881	3.9881	11.4799	0	PROCESSED	57541.4170833333	2016-06-02 10:00:36	54912	2009-03-22 00:00:00	54546.2311574074	2008-03-21 05:32:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063160/	Quick Look
27	GALACTIC CENTER	265.3803	-29.7558	264.581055	-29.731436	265.955939	-6.379444	358.83357751	0.33021849	269	54016.4324074074	2006-10-08 10:22:40	54017.0968055556	2006-10-09 02:19:24	501049010	19.5627	20	19.5627	19.5627	19.5627	19.5627	2	2	2	2	1	0	0	17.6336	17.6336	57.3959	1	PROCESSED	57535.7944675926	2016-05-27 19:04:02	54735	2008-09-26 00:00:00	54053.4403356482	2006-11-14 10:34:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501049010/	Quick Look
28	COMET_8P_TUTTLE-P1-8	28.3076	6.2429	27.652953	5.997039	28.526064	-5.034788	149.32011202	-53.43313536	248.4984	54470.9825	2008-01-05 23:34:48	54471.0487384259	2008-01-06 01:10:11	502062080	3.219	3.2	3.219	3.219	0	3.219	1	1	0	1	1	0	0	3.374	3.374	5.664	0	PROCESSED	57541.0065046296	2016-06-02 00:09:22	54908	2009-03-18 00:00:00	54542.2264583333	2008-03-17 05:26:06	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062080/	Quick Look
29	RCW86_WEST	220.2753	-62.427	219.29491	-62.212988	240.606158	-43.963376	315.24703456	-2.20673417	96.1553	54864.7563194444	2009-02-02 18:09:06	54866.0134259259	2009-02-04 00:19:20	503001010	53.5519	50	53.5519	53.5519	0	53.5519	2	2	0	2	1	0	0	48.9081	48.9081	108.602	1	PROCESSED	57545.4580324074	2016-06-06 10:59:34	55329	2010-05-13 00:00:00	54880.570462963	2009-02-18 13:41:28	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030011	Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		JAP	3	AO3	RCW86 MAPPING OBSERVATION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503001010/	Quick Look
30	CYGNUS LOOP (P20)	311.9894	31.1824	311.473917	30.997098	326.586885	46.721175	73.97872298	-7.73281487	50.0002	54596.7397685185	2008-05-10 17:45:16	54597.51	2008-05-11 12:14:24	503056010	30.1129	25	30.1129	30.1343	0	30.1209	2	2	0	2	1	0	0	27.2057	27.2057	66.5339	0	PROCESSED	57545.8695023148	2016-06-06 20:52:05	54972	2009-05-21 00:00:00	54606.1121759259	2008-05-20 02:41:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503056010/	Quick Look
31	RCW 86	221.2555	-62.3618	220.269135	-62.150858	241.140538	-43.714444	315.68741681	-2.33681001	278.3377	53959.4574652778	2006-08-12 10:58:45	53961.1294907407	2006-08-14 03:06:28	501037010	59.8054	60	59.8294	59.8054	59.8294	59.8214	2	2	2	2	1	0	0	54.405	54.405	144.42	1	PROCESSED	57535.2984259259	2016-05-27 07:09:44	54394	2007-10-21 00:00:00	54021.0740972222	2006-10-13 01:46:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010054	We propose an observation of the Northwest region of RCW 86, one of Galactic supernova remnants (SNRs). Hard X-ray continuum of RCW 86 is accompanied by Fe K line emission at 6.4keV. There is strong possibility that the origin of this line is electrons and protons accelerated in the shell of the SNR. In PV phase, the Southeast region of RCW 86 will be observed, and the density of this region is much larger than that of the Northwest region. Therefore we must compare the fluxes of Fe line and hard continuum of both regions, and discuss the correlation between the flux and the density of emitting region. Such comparative study is very useful for understanding the particle acceleration in the shell-like SNRs.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		JAP	1	AO1	RCW 86:PECULIAR SNR WITH NEUTRAL FE K LINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501037010/	Quick Look
32	VELA JR P30	134.1665	-46.7036	133.737948	-46.510338	161.294913	-59.700207	267.059354	-0.84402772	347.0006	54654.7208449074	2008-07-07 17:18:01	54655.0844328704	2008-07-08 02:01:35	503042010	10.1159	10	10.1159	10.1159	0	10.1159	2	2	0	2	1	0	0	10.0536	10.0536	31.3839	0	PROCESSED	57542.9967592593	2016-06-03 23:55:20	55048	2009-08-05 00:00:00	54679.397962963	2008-08-01 09:33:04	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503042010/	Quick Look
33	ERIDANUS HOLE	67.1401	-17.0746	66.578414	-17.184035	61.759444	-38.302767	213.43674881	-39.09232011	64.2755	54311.0359606482	2007-07-30 00:51:47	54313.2161921296	2007-08-01 05:11:19	502076010	103.7523	100	103.7523	103.7523	0	103.7523	2	2	0	2	1	0	0	92.2091	92.2091	188.3518	2	PROCESSED	57539.4003356482	2016-05-31 09:36:29	54710	2008-09-01 00:00:00	54340.7341898148	2007-08-28 17:37:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021224	We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source.	GALACTIC DIFFUSE EMISSION	5	B	MASSIMILIANO GALEAZZI		USA	2	AO2	STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502076010/	Quick Look
34	RXJ1713-3946	258.1672	-39.4231	257.303004	-39.36394	260.487659	-16.371231	347.50735004	-0.13585591	267.9988	53989.9221643518	2006-09-11 22:07:55	53990.3106712963	2006-09-12 07:27:22	501065010	22.011	20	22.011	22.011	22.011	22.011	2	2	2	2	1	0	0	20.7973	20.7973	33.5579	0	PROCESSED	57535.5534606482	2016-05-27 13:16:59	54526	2008-03-01 00:00:00	54020.8390162037	2006-10-12 20:08:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501065010/	Quick Look
35	GC SGR D	267.0913	-27.9356	266.303192	-27.919557	267.412914	-4.520645	1.16847417	0.00287016	108.7996	54174.7887847222	2007-03-15 18:55:51	54176.2127199074	2007-03-17 05:06:19	501059010	62.2372	63	62.2372	62.2452	0	62.2452	2	2	0	2	1	0	0	54.3697	54.3697	123.028	0	PROCESSED	57537.7233912037	2016-05-29 17:21:41	54736	2008-09-27 00:00:00	54185.4865740741	2007-03-26 11:40:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501059010/	Quick Look
36	ASO0078	59.472	32.09	58.682067	31.946958	63.963224	11.368156	162.76236061	-16.0043339	83.0007	55045.8202777778	2009-08-02 19:41:12	55046.3273032407	2009-08-03 07:51:19	504041010	21.312	20	21.32	21.32	0	21.312	1	1	0	1	1	0	0	21.2959	21.2959	43.7999	0	PROCESSED	57548.0349074074	2016-06-09 00:50:16	55430	2010-08-22 00:00:00	55064.0383912037	2009-08-21 00:55:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 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 DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504041010/	Quick Look
37	CYGNUS_LOOP_P17	312.199	30.014	311.677424	29.82795	326.178147	45.573278	73.16561663	-8.59879153	61.9999	53877.7613657407	2006-05-22 18:16:22	53878.0446064815	2006-05-23 01:04:14	501034010	14.1953	14	14.1993	14.2033	14.1993	14.1953	2	2	2	2	1	0	0	14.8231	14.8231	24.464	0	PROCESSED	57534.3944328704	2016-05-26 09:27:59	54394	2007-10-21 00:00:00	53926.1395833333	2006-07-10 03:21:00	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501034010/	Quick Look
38	JUPITER	103.8837	23.1078	103.127442	23.17281	102.752218	0.279385	192.54363279	11.16228902	264.4065	56762.7225115741	2014-04-15 17:20:25	56763.066099537	2014-04-16 01:35:11	508023030	8.9125	160	8.9125	8.9125	0	8.9125	2	2	0	2	1	0	0	6.9063	6.9063	22.6469	0	PROCESSED	57614.254212963	2016-08-14 06:06:04	57212	2015-07-09 00:00:00	56833.5559722222	2014-06-25 13:20:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023030/	Quick Look
39	HESSJ1741-B	265.2407	-30.3098	264.437915	-30.284751	265.852586	-6.937089	358.29952005	0.1396669	74.0024	54888.0423611111	2009-02-26 01:01:00	54889.4828587963	2009-02-27 11:35:19	503077010	51.2616	50	51.2696	51.2616	0	51.2696	2	2	0	2	1	0	0	43.7072	43.7072	124.4239	1	PROCESSED	57545.6763773148	2016-06-06 16:13:59	55330	2010-05-14 00:00:00	54908.5791550926	2009-03-18 13:53:59	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030113	HESSJ1741-302 is one of the most darkest TeV unidentified objects which was discovered with the H.E.S.S. telescope recently. The location strongly suggests that the object is physically connected to the diffuse TeV gamma-ray emission along the Galactic plane. On the other hand, there is a pulsar near the object, and it may be an off-set pulsar wind nebula. To clarify the origin of the object, we propose to the observation of HESSJ1741.	GALACTIC DIFFUSE EMISSION	5	C	HIRONORI MATSUMOTO		JAP	3	AO3	DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503077010/	Quick Look
40	JUPITER	104.3715	23.0706	103.615684	23.137913	103.202438	0.28593	192.77027841	11.55390373	264.582	56766.448287037	2014-04-19 10:45:32	56766.781400463	2014-04-19 18:45:13	508023090	11.9454	160	11.9534	11.9454	0	11.9614	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57614.9588773148	2016-08-14 23:00:47	57212	2015-07-09 00:00:00	56782.506099537	2014-05-05 12:08:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023090/	Quick Look
41	GRXE_E_10	267.9015	-25.9408	267.12546	-25.928719	268.101648	-2.513628	3.25115356	0.4070413	105.0001	56362.3793865741	2013-03-11 09:06:19	56364.8778472222	2013-03-13 21:04:06	507075010	101.3428	100	101.3428	101.3428	0	101.3428	2	2	0	2	1	0	0	88.2422	88.2422	215.806	2	PROCESSED	57610.8450462963	2016-08-10 20:16:52	56018	2012-04-01 00:00:00	56377.5882175926	2013-03-26 14:07:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507075010/	Quick Look
42	MBM16	49.7694	11.5801	49.085806	11.399029	50.444533	-6.508969	170.60605682	-37.27197306	254.9211	56331.4284606482	2013-02-08 10:16:59	56333.553587963	2013-02-10 13:17:10	507076020	80.9506	80	80.9746	80.9506	0	80.9746	2	2	0	2	1	0	0	69.3076	69.3076	183.5839	2	PROCESSED	57610.5874074074	2016-08-10 14:05:52	56018	2012-04-01 00:00:00	56349.5813657407	2013-02-26 13:57:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076003	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	7	AO7	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507076020/	Quick Look
43	VELA JR P27	133.2844	-46.6061	132.858246	-46.415943	160.180564	-59.949881	266.59417196	-1.24373956	347.0008	54653.8375925926	2008-07-06 20:06:08	54654.1668865741	2008-07-07 04:00:19	503039010	11.0337	10	11.0417	11.0417	0	11.0337	1	1	0	1	1	0	0	11.3372	11.3372	28.4479	0	PROCESSED	57542.9844560185	2016-06-03 23:37:37	55048	2009-08-05 00:00:00	54679.3497222222	2008-08-01 08:23:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503039010/	Quick Look
44	SGR D SNR	267.1922	-28.1274	266.402882	-28.111843	267.506075	-4.710631	1.05009547	-0.17236121	267.8977	54349.018599537	2007-09-06 00:26:47	54352.6738310185	2007-09-09 16:10:19	502020010	139.0808	133	139.0808	139.0808	0	139.0808	2	2	0	2	1	0	0	124.5025	124.5025	315.7798	1	PROCESSED	57540.026087963	2016-06-01 00:37:34	54776	2008-11-06 00:00:00	54371.5203472222	2007-09-28 12:29:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020031	We propose a 100 ksec observation of the Sgr D region. This region contains a supernova remnant (SNR), a massive molecular cloud, an HII region and diffuse TeV gamma-ray emission. The objectives are to detect Sgr D SNR and diffuse X-rays from the TeV source, to discover new SNRs and X-ray Reflection Nebulae (XRNe), and to investigate the spatial distribution of high temperature plasma connecting the Galactic center and the Galactic ridge regions.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	2	AO2	OBSERVATIONS OF SGR D SNR, A TEV SOURCE AND DIFFUSE X-RAYS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502020010/	Quick Look
45	HESSJ1857-A	284.2126	2.7519	283.584668	2.685017	285.744612	25.418977	35.99783049	0.0515802	269.8116	55822.9197800926	2011-09-18 22:04:29	55823.984212963	2011-09-19 23:37:16	506019010	40.9249	40	40.9249	40.9249	0	40.9249	2	2	0	2	1	0	0	35.8469	35.8469	91.9279	1	PROCESSED	57603.2046180556	2016-08-03 04:54:39	56233	2012-11-02 00:00:00	55865.2326157407	2011-10-31 05:34:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060061	Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	6	AO6	ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506019010/	Quick Look
46	IC 443	94.2974	22.7535	93.540286	22.772525	93.964523	-0.628288	188.8890151	3.10517693	91.6993	56197.2290277778	2012-09-27 05:29:48	56199.7780324074	2012-09-29 18:40:22	507015010	101.8023	400	101.8103	101.8023	0	101.8103	2	2	0	2	1	0	0	91.994	91.994	220.1877	0	PROCESSED	57607.2728472222	2016-08-07 06:32:54	56018	2012-04-01 00:00:00	56225.5965162037	2012-10-25 14:18:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070015	The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	7	AO7	DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA --	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015010/	Quick Look
47	FERMI_BUBBLE_N4	233.8333	7.0797	233.2207	7.24518	229.504794	25.578453	13.3126084	46.30488493	287.5	56146.4387268518	2012-08-07 10:31:46	56146.9862615741	2012-08-07 23:40:13	507004010	20.9469	20	20.9509	20.9469	0	20.9549	2	2	0	2	1	0	0	20.7048	20.7048	47.306	2	PROCESSED	57606.7955787037	2016-08-06 19:05:38	56535	2013-08-31 00:00:00	56169.0484375	2012-08-30 01:09:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507004010/	Quick Look
48	BULGE 3	274.7046	-31.4846	273.893726	-31.505472	274.041648	-8.109784	1.3002625	-7.49777303	80.4025	53800.3437962963	2006-03-06 08:15:04	53801.7474421296	2006-03-07 17:56:19	500001010	51.8468	50	51.8548	51.8548	51.8548	51.8468	2	2	2	2	1	0	0	45.0783	45.0783	121.2459	0	PROCESSED	57533.1540972222	2016-05-25 03:41:54	54247	2007-05-27 00:00:00	54041.7128703704	2006-11-02 17:06:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001014	Leading .	GALACTIC DIFFUSE EMISSION	5	A	DAN MCCAMMON		JAP	0	SWG	THE SOFT GALACTIC BULGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500001010/	Quick Look
49	SN1006 NW	225.6364	-41.8003	224.819551	-41.604176	235.339658	-23.546444	327.59294648	14.70833496	115.0008	53766.4881365741	2006-01-31 11:42:55	53767.55375	2006-02-01 13:17:24	500017010	53.0194	50	53.0194	53.0277	53.0273	53.0273	2	2	2	2	1	0	0	60.4123	60.4123	92.0679	0	PROCESSED	57532.8347685185	2016-05-24 20:02:04	54247	2007-05-27 00:00:00	54040.7669675926	2006-11-01 18:24:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001062	We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		JAP	0	SWG	THE EJECTA IN SN1006	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500017010/	Quick Look
50	GC15	266.9617	-29.4257	266.164223	-29.409004	267.329759	-6.012747	359.83382525	-0.66952641	260.7835	54383.1536226852	2007-10-10 03:41:13	54383.6391666667	2007-10-10 15:20:24	502003010	21.4671	20	21.4751	21.4671	0	21.4751	2	2	0	2	1	0	0	18.9225	18.9225	41.9439	0	PROCESSED	57540.2312731482	2016-06-01 05:33:02	54771	2008-11-01 00:00:00	54402.7485532407	2007-10-29 17:57:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502003010/	Quick Look
51	VELA JR P2	132.1691	-45.7748	131.740578	-45.588644	157.998003	-59.663034	265.4613949	-1.31133586	347.0033	54285.6908217593	2007-07-04 16:34:47	54285.9036342593	2007-07-04 21:41:14	502024010	10.8502	10	10.8742	10.8662	0	10.8502	1	1	0	1	1	0	0	9.6037	9.6037	18.3759	0	PROCESSED	57539.0914467593	2016-05-31 02:11:41	54696	2008-08-18 00:00:00	54328.4167361111	2007-08-16 10:00:06	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502024010/	Quick Look
52	VELA JR P33	133.4681	-47.1616	133.045488	-46.970785	161.00407	-60.345222	267.10091899	-1.50393046	347.0007	54655.5652777778	2008-07-08 13:34:00	54656.0084837963	2008-07-09 00:12:13	503045010	12.0155	10	12.0155	12.0155	0	12.0155	2	2	0	2	1	0	0	11.0116	11.0116	38.2899	0	PROCESSED	57543.0047106482	2016-06-04 00:06:47	55048	2009-08-05 00:00:00	54679.4195601852	2008-08-01 10:04:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503045010/	Quick Look
53	MBM36	238.3613	-4.7912	237.701072	-4.643799	237.20756	15.120262	4.0047136	35.6981582	275.8793	56894.6980324074	2014-08-25 16:45:10	56896.6598958333	2014-08-27 15:50:15	509074010	83.1887	80	83.1967	83.1887	0	83.1967	2	2	0	2	1	0	0	3.755	3.755	8.94	0	PROCESSED	57616.559525463	2016-08-16 13:25:43	56748	2014-04-01 00:00:00	56929.2087615741	2014-09-29 05:00:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096001	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	9	AO9	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509074010/	Quick Look
54	GB_NORTH_4	264.8998	-28.3109	264.109826	-28.284233	265.484852	-4.949634	359.83607677	1.45248781	106.6967	57110.9717708333	2015-03-29 23:19:21	57113.0203472222	2015-04-01 00:29:18	509080010	88.1941	100	88.1941	95.0455	0	95.0615	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8835648148	2016-08-17 21:12:20	56748	2014-04-01 00:00:00	57125.4051736111	2015-04-13 09:43:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096002	The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	9	AO9	MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY-	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509080010/	Quick Look
55	CYGNUS_LOOP_P10	311.5744	30.3992	311.055864	30.215413	325.67249	46.135207	73.13474548	-7.93635975	240.0007	54417.2506944444	2007-11-13 06:01:00	54417.6043402778	2007-11-13 14:30:15	501020010	16.7958	10	16.7958	16.8198	0	16.8038	2	2	0	2	1	0	0	12.6729	12.6729	30.5499	0	PROCESSED	57540.5008333333	2016-06-01 12:01:12	54798	2008-11-28 00:00:00	54430.1578472222	2007-11-26 03:47:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501020010/	Quick Look
56	PUP A : INTERIOR	125.5916	-42.8951	125.161363	-42.733897	147.106586	-59.478577	260.333956	-3.34905821	276.8883	53842.5813541667	2006-04-17 13:57:09	53842.9127199074	2006-04-17 21:54:19	501088010	20.2709	20	20.2924	20.2949	20.2789	20.2709	1	1	1	1	1	0	0	19.9519	19.9519	28.6239	0	PROCESSED	57533.5042476852	2016-05-25 12:06:07	54401	2007-10-28 00:00:00	53906.8948611111	2006-06-20 21:28:36	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501088010/	Quick Look
57	CTB109 NOTHWEST	345.2638	59.0349	344.742477	58.766045	23.94959	57.015916	109.14185824	-0.84931137	252.0017	55908.2838078704	2011-12-13 06:48:41	55909.1988078704	2011-12-14 04:46:17	506037010	40.7488	40	40.7488	40.7568	0	40.7648	2	2	0	2	1	0	0	39.201	39.201	79.044	0	PROCESSED	57604.1345601852	2016-08-04 03:13:46	56288	2012-12-27 00:00:00	55921.0397685185	2011-12-26 00:57:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060100	Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations.	GALACTIC DIFFUSE EMISSION	5	C	TOSHIO NAKANO		JAP	6	AO6	SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506037010/	Quick Look
58	OFF-FIELD2	312.2284	-9.8925	311.551158	-10.078408	311.903273	7.617962	37.42106637	-30.55240738	73.668	56784.946724537	2014-05-07 22:43:17	56787.0627314815	2014-05-10 01:30:20	509043010	80.156	80	80.156	80.156	0	80.156	2	2	0	2	1	0	0	69.6142	69.6142	182.8079	1	PROCESSED	57615.1427430556	2016-08-15 03:25:33	56748	2014-04-01 00:00:00	56861.5828240741	2014-07-23 13:59:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091321	Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma.	GALACTIC DIFFUSE EMISSION	5	A	ANJALI GUPTA		USA	9	AO9	CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509043010/	Quick Look
59	CTB109 SOUTHEAST	345.764	58.7015	345.237296	58.43203	23.8569	56.597018	109.24155205	-1.25930647	252.0022	55910.7526851852	2011-12-15 18:03:52	55911.4007638889	2011-12-16 09:37:06	506040010	30.4455	30	30.4455	30.4455	0	30.4455	2	2	0	2	1	0	0	28.7511	28.7511	55.9879	1	PROCESSED	57604.1444212963	2016-08-04 03:27:58	56289	2012-12-28 00:00:00	55922.0080555556	2011-12-27 00:11:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060100	Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations.	GALACTIC DIFFUSE EMISSION	5	C	TOSHIO NAKANO		JAP	6	AO6	SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506040010/	Quick Look
60	HESS J1356-645 1	209.4297	-64.5068	208.507718	-64.263148	235.862386	-48.071536	309.98959301	-2.54712319	106.5083	56318.4192939815	2013-01-26 10:03:47	56320.0002083333	2013-01-28 00:00:18	507019010	55.7489	50	55.762	55.7569	0	55.7489	2	2	0	2	1	0	0	65.1023	65.1023	136.5678	2	PROCESSED	57608.6328587963	2016-08-08 15:11:19	56708	2014-02-20 00:00:00	56342.6666319444	2013-02-19 15:59:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070017	Recently, pulsar wind nebulae is focused on one of the electron accelerators in our Galaxy. Especially TeV pulsar wind nebulae are supposed to have a largely extended X-ray emission. Since the X-ray emission is much larger than the size considering the typical electron lifetime, high energy electrons strangely seem to be transferred too fast or without cooling. To study the electron diffusion of young pulsar wind nebula, we propose observations of HESS J1356-645, which is off the Galactic plane and is free from the Galactic ridge X-ray emission.	GALACTIC DIFFUSE EMISSION	5	C	TAKAHISA FUJINAGA		JAP	7	AO7	OFF-PLANE TEV GAMMA-RAY SOURCE HESS J1356-645	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507019010/	Quick Look
61	SN1006_SE1	225.8641	-42.0384	225.045074	-41.843059	235.594631	-23.72201	327.62177329	14.41744154	286.0629	56883.8521064815	2014-08-14 20:27:02	56887.5210648148	2014-08-18 12:30:20	509082010	201.8322	480	201.8322	202.4881	0	202.5201	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5228240741	2016-08-16 12:32:52	56748	2014-04-01 00:00:00	56910.6390509259	2014-09-10 15:20:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096004	We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		USA	9	AO9	THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509082010/	Quick Look
62	SN1006_SE1	225.857	-42.039	225.037992	-41.843634	235.58934	-23.724178	327.61674963	14.4195613	107.6985	57063.4521643518	2015-02-10 10:51:07	57069.9807060185	2015-02-16 23:32:13	509082020	258.382	280	258.382	278.7901	0	278.8541	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6457523148	2016-08-17 15:29:53	56748	2014-04-01 00:00:00	57080.4416898148	2015-02-27 10:36:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096004	We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		USA	9	AO9	THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509082020/	Quick Look
63	H2356_VICINITY_A	359.8969	-30.2089	359.255002	-30.487352	346.863445	-27.454803	14.71906615	-78.22459894	68.0006	55696.8464583333	2011-05-15 20:18:54	55698.0938773148	2011-05-17 02:15:11	506028010	52.1657	50	52.1657	52.1657	0	52.1657	2	2	0	2	1	0	0	46.5791	46.5791	107.7539	1	PROCESSED	57602.0723148148	2016-08-02 01:44:08	56075	2012-05-28 00:00:00	55708.0697106482	2011-05-27 01:40:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060075	We propose to observe the two vicinities of H2356-309 for 50 ks each. Absorption lines from ions at z=0 and z=0.03 has been observed with grating spectrometers in the spectrum of H2356-309. Emission analysis with Suzaku will provide independent information on the medium responsible for the absorption lines. By combining the emission surface brightness and aborption equivalent width, we will constrain the temperature and physical length of the interstellar and intergalactic medium.	GALACTIC DIFFUSE EMISSION	5	A	YOH TAKEI		JAP	6	AO6	EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC AND INTERGALACTIC WARM-HOT GAS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506028010/	Quick Look
64	H2356_VICINITY_B	359.9868	-29.9493	359.345168	-30.227755	347.07269	-27.257526	15.89682365	-78.35224854	69.5008	55698.0951388889	2011-05-17 02:17:00	55699.3474305556	2011-05-18 08:20:18	506029010	51.4072	50	51.4312	51.4232	0	51.4072	2	2	0	2	1	0	0	42.546	42.546	108.1559	1	PROCESSED	57602.0868402778	2016-08-02 02:05:03	56075	2012-05-28 00:00:00	55708.1035069444	2011-05-27 02:29:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060075	We propose to observe the two vicinities of H2356-309 for 50 ks each. Absorption lines from ions at z=0 and z=0.03 has been observed with grating spectrometers in the spectrum of H2356-309. Emission analysis with Suzaku will provide independent information on the medium responsible for the absorption lines. By combining the emission surface brightness and aborption equivalent width, we will constrain the temperature and physical length of the interstellar and intergalactic medium.	GALACTIC DIFFUSE EMISSION	5	A	YOH TAKEI		JAP	6	AO6	EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC AND INTERGALACTIC WARM-HOT GAS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506029010/	Quick Look
65	HESS_J1809-193_S	272.3365	-19.5311	271.597005	-19.540657	272.197453	3.891828	10.84429394	0.04252392	106.4999	54557.6901851852	2008-04-01 16:33:52	54558.6161805556	2008-04-02 14:47:18	503079010	44.2481	40	44.2481	44.2481	0	44.2481	2	2	0	2	1	0	0	32.2142	32.2142	79.9698	1	PROCESSED	57542.0277546296	2016-06-03 00:39:58	54950	2009-04-29 00:00:00	54570.1866666667	2008-04-14 04:28:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030126	A survey of the Galactic plane with H.E.S.S. has revealed the existance of several new very-high-energy (VHE) gamma-ray sources. As gamma rays are produced by interactions of relativistic particles, observing VHE emission reveals the acceleration sites of particles. Although it had been thought that such acceleration occur in the shock of SNR, it became clear that several VHE sources are pulsar wind nebulae (PWNe). This indicates that PWNe are also the acceleration sites of particles. HESS J1809-193 is a diffuse and a pulsar wind nebula candidate source, but details of the VHE emission mechanisms have been unclear yet. With the high sensitivity of XIS, we investigate spatial distribution of the spectrum around HESS J1809-193 and reveal its nature and the VHE emission mechanism.	GALACTIC DIFFUSE EMISSION	5	A	TAKAYASU ANADA		JAP	3	AO3	INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503079010/	Quick Look
66	CYG_BGD1	306.6527	39.4856	306.195949	39.320312	325.617981	56.073001	78.0015669	0.73572902	218.9004	56280.1666666667	2012-12-19 04:00:00	56280.6286458333	2012-12-19 15:05:15	507041010	26.9324	25	26.9404	26.9324	0	26.9404	1	1	0	1	1	0	0	20.4527	20.4527	39.9119	0	PROCESSED	57608.3151273148	2016-08-08 07:33:47	56683	2014-01-26 00:00:00	56316.5312268518	2013-01-24 12:44:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070060	The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object.	GALACTIC DIFFUSE EMISSION	5	C	TSUNEFUMI MIZUNO		JAP	7	AO7	SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507041010/	Quick Look
67	GALACTIC_BULGE1	267.2201	-29.3677	266.422949	-29.352259	267.554885	-5.950193	359.99969448	-0.83243485	274.7	55118.4798148148	2009-10-14 11:30:56	55119.6453587963	2009-10-15 15:29:19	504088010	47.23	50	47.23	47.23	0	47.23	2	2	0	2	1	0	0	32.6139	32.6139	100.7	2	PROCESSED	57548.8825231482	2016-06-09 21:10:50	54922	2009-04-01 00:00:00	55134.0688425926	2009-10-30 01:39:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504088010/	Quick Look
68	GALACTIC_BULGE9	267.6768	-31.2805	266.867115	-31.267244	267.986252	-7.855618	358.55970985	-2.15232996	265.3076	55090.3066550926	2009-09-16 07:21:35	55091.5758564815	2009-09-17 13:49:14	504092010	50.9199	50	50.9439	50.9359	0	50.9199	2	2	0	2	1	0	0	45.5744	45.5744	109.6459	1	PROCESSED	57548.6135069444	2016-06-09 14:43:27	54922	2009-04-01 00:00:00	55109.4315740741	2009-10-05 10:21:28	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504092010/	Quick Look
69	JUPITER	103.8407	23.1129	103.084394	23.177707	102.712362	0.280692	192.5219391	11.12856775	264.3937	56762.3891782407	2014-04-15 09:20:25	56762.7223611111	2014-04-15 17:20:12	508023020	15.4083	160	15.4083	15.4083	0	15.4083	1	1	0	1	1	0	0	12.2744	12.2744	28.7839	1	PROCESSED	57614.2553819445	2016-08-14 06:07:45	57212	2015-07-09 00:00:00	56778.6154166667	2014-05-01 14:46:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023020/	Quick Look
70	BULGE 6	282.6839	-33.8925	281.860158	-33.951684	280.687841	-10.9215	1.99857856	-14.59644221	88.3467	53802.7373032407	2006-03-08 17:41:43	53803.0466087963	2006-03-09 01:07:07	500003010	14.2617	10	14.2617	14.2617	14.2617	14.2617	2	2	2	2	1	0	0	11.414	11.414	26.7159	1	PROCESSED	57533.1570833333	2016-05-25 03:46:12	54247	2007-05-27 00:00:00	54041.7424305556	2006-11-02 17:49:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001014	Leading .	GALACTIC DIFFUSE EMISSION	5	A	DAN MCCAMMON		JAP	0	SWG	THE SOFT GALACTIC BULGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500003010/	Quick Look
71	RXJ1713-3946_ID3	258.1658	-40.0306	257.296734	-39.971421	260.540524	-16.976597	347.01547145	-0.49239611	87.0009	55244.1262847222	2010-02-17 03:01:51	55244.4779398148	2010-02-17 11:28:14	504029010	20.8716	20	20.9036	20.9036	0	20.8716	1	1	0	1	1	0	0	20.8868	20.8868	30.3759	0	PROCESSED	57550.6116087963	2016-06-11 14:40:43	55622	2011-03-02 00:00:00	55256.0720601852	2010-03-01 01:43:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040021	We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009.	GALACTIC DIFFUSE EMISSION	5	B	TADAYUKI TAKAHASHI		JAP	4	AO4	STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504029010/	Quick Look
72	HOT BLOB 2	131.2547	53.3234	130.330211	53.505247	118.317658	33.861433	164.89716269	38.20704104	284.8982	57137.3573842593	2015-04-25 08:34:38	57139.1293055556	2015-04-27 03:06:12	509008010	46.0224	80	46.0224	77.9795	0	78.0115	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.041412037	2016-08-18 00:59:38	57520	2016-05-12 00:00:00	57154.4516087963	2015-05-12 10:50:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090044	Hot blobs including plasma of temperature kT = 0.6 - 1.0 keV in the Milky-Way Halo were found in 1/10 of the sky by systematical analysis of the soft X-ray diffuse background in Suzaku/XIS observations. They can play a role in matter and energy transportation among the Galactic plane, the Milky-Way Halo and intergalactic space. In order to reveal origin and physical condition of them, we focus on the part of a hot blob in (ell, b) = (161.505, 40.696) and propose to observe neighboring this area to constrain its size.	GALACTIC DIFFUSE EMISSION	5	C	NORIO SEKIYA		JAP	9	AO9	ORIGIN AND PHYSICAL CONDITION OF HOT BLOBS IN THE MILKY-WAY HALO	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509008010/	Quick Look
73	IC 443	94.3028	22.7465	93.545727	22.765551	93.96971	-0.635136	188.89754986	3.10625906	259.0005	56378.1771527778	2013-03-27 04:15:06	56379.6668865741	2013-03-28 16:00:19	507015020	59.2712	300	59.2712	59.2712	0	59.2712	2	2	0	2	1	0	0	51.2705	51.2705	128.6878	3	PROCESSED	57610.9601388889	2016-08-10 23:02:36	56018	2012-04-01 00:00:00	56391.749224537	2013-04-09 17:58:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070015	The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	7	AO7	DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA --	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015020/	Quick Look
74	LOW_LATITUDE_97-10	311.8076	60.1112	311.52726	59.92615	0.701483	70.601802	96.61384914	10.40907029	101.0346	54571.1324652778	2008-04-15 03:10:45	54572.8890509259	2008-04-16 21:20:14	503075010	79.8119	80	79.8199	79.8279	0	79.8119	2	2	0	2	1	0	0	80.8105	80.8105	151.7498	2	PROCESSED	57542.342962963	2016-06-03 08:13:52	54953	2009-05-02 00:00:00	54581.3271643518	2008-04-25 07:51:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030105	Suzaku observations of diffuse background emission indicate galactic-latitude dependence of OVII intensity. The result of our AO-2 observation strongly supports this dependence. This suggests that the major part of the emission is originating from the halo or the extended disk of our galaxy. In order to confirm the galactic-latitude dependency and to constrain the spatial distribution of the OVII emitting gas, we propose to observe diffuse radiation at a low galactic latitude of ~ 10 deg.	GALACTIC DIFFUSE EMISSION	5	B	TOMOTAKA YOSHINO		JAP	3	AO3	RESOLVING LARGE-SCALE SPATIAL DEPENDENCE OF SOFT X-RAY DIFFUSE EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503075010/	Quick Look
75	IC 443	94.2972	22.4797	93.541644	22.498727	93.972502	-0.901975	189.13057055	2.97563306	274.0001	54166.5158680556	2007-03-07 12:22:51	54167.612025463	2007-03-08 14:41:19	501006020	44.0135	40	44.0135	44.0375	0	44.0215	2	2	0	2	1	0	0	36.3209	36.3209	94.6999	1	PROCESSED	57537.6255324074	2016-05-29 15:00:46	54736	2008-09-27 00:00:00	54172.2247800926	2007-03-13 05:23:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010040	IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution.	GALACTIC DIFFUSE EMISSION	5	B	MASANOBU OZAKI		JAP	1	AO1	UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501006020/	Quick Look
76	73P/SW3	279.6627	33.4734	279.203358	33.427762	284.650097	56.423756	62.35168426	17.03145652	46.5564	53862.4804282407	2006-05-07 11:31:49	53862.5419444444	2006-05-07 13:00:24	500012020	3.248	5	3.248	3.248	3.248	3.248	1	1	1	1	1	0	0	2.1119	2.1119	5.2799	0	PROCESSED	57533.7332407407	2016-05-25 17:35:52	54256	2007-06-05 00:00:00	54042.2282175926	2006-11-03 05:28:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500012020/	Quick Look
77	73P/SW3	316.717	24.6807	316.164001	24.478965	328.484877	39.12074	71.53645371	-15.07849931	72.7087	53868.1752314815	2006-05-13 04:12:20	53868.2085532407	2006-05-13 05:00:19	500013010	2.353	20	2.353	2.353	2.353	2.353	1	1	1	1	1	0	0	2.595	2.595	2.8719	0	PROCESSED	57534.2831597222	2016-05-26 06:47:45	54256	2007-06-05 00:00:00	54042.2312268518	2006-11-03 05:32:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013010/	Quick Look
78	73P/SW3	317.1042	24.5187	316.549923	24.315676	328.827114	38.838912	71.64340536	-15.45205291	72.7099	53868.2091666667	2006-05-13 05:01:12	53868.2752199074	2006-05-13 06:36:19	500013020	3.225	20	3.225	3.225	3.225	3.225	1	1	1	1	1	0	0	3.467	3.467	5.7039	0	PROCESSED	57534.2879398148	2016-05-26 06:54:38	54256	2007-06-05 00:00:00	54042.2634027778	2006-11-03 06:19:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013020/	Quick Look
79	73P/SW3	319.1503	23.6322	318.589279	23.422515	330.602424	37.314629	72.21442919	-17.44595626	72.7095	53868.5425	2006-05-13 13:01:12	53868.6085532407	2006-05-13 14:36:19	500013070	3.0624	20	3.0624	3.0624	3.0624	3.0624	1	1	1	1	1	0	0	2.088	2.088	5.688	1	PROCESSED	57534.3049074074	2016-05-26 07:19:04	54256	2007-06-05 00:00:00	54042.3037268518	2006-11-03 07:17:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013070/	Quick Look
80	73P/SW3	17.8447	-9.1515	17.217751	-9.416998	12.842123	-15.443966	138.54867442	-71.41609802	59.3994	53893.7363888889	2006-06-07 17:40:24	53893.8023032407	2006-06-07 19:15:19	500014020	3.2369	35	3.2369	3.2369	3.2369	3.2369	1	1	1	1	1	0	0	2.478	2.478	5.6879	0	PROCESSED	57534.5816435185	2016-05-26 13:57:34	54267	2007-06-16 00:00:00	54052.5079861111	2006-11-13 12:11:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014020/	Quick Look
81	73P/SW3	18.0085	-9.2093	17.381763	-9.474557	12.972897	-15.560645	139.0853548	-71.43220951	59.4015	53893.9358333333	2006-06-07 22:27:36	53894.0023032407	2006-06-08 00:03:19	500014050	3.235	35	3.235	3.235	3.235	3.235	1	1	1	1	1	0	0	2.5041	2.5041	5.7359	0	PROCESSED	57534.5878125	2016-05-26 14:06:27	54267	2007-06-16 00:00:00	54052.5317361111	2006-11-13 12:45:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014050/	Quick Look
82	73P/SW3	18.1094	-9.2436	17.482792	-9.508708	13.054019	-15.631304	139.41528011	-71.44015907	59.3996	53894.0691666667	2006-06-08 01:39:36	53894.1356365741	2006-06-08 03:15:19	500014070	2.2209	35	2.2209	2.2209	2.2209	2.2209	1	1	1	1	1	0	0	1.939	1.939	5.7359	1	PROCESSED	57534.589849537	2016-05-26 14:09:23	54267	2007-06-16 00:00:00	54052.5472800926	2006-11-13 13:08:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014070/	Quick Look
83	73P/SW3	18.2503	-9.299	17.623885	-9.563897	13.164284	-15.736856	139.88257526	-71.45759255	59.3985	53894.2691435185	2006-06-08 06:27:34	53894.3356134259	2006-06-08 08:03:17	500014100	1.3121	35	1.3121	1.3121	1.3121	1.3121	1	1	1	1	1	0	0	1.322	1.322	5.742	0	PROCESSED	57534.5960185185	2016-05-26 14:18:16	54267	2007-06-16 00:00:00	54052.5405324074	2006-11-13 12:58:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014100/	Quick Look
84	73P/SW3	18.435	-9.3697	17.808837	-9.63432	13.309685	-15.873419	140.49459076	-71.47695116	59.4003	53894.5358333333	2006-06-08 12:51:36	53894.6016087963	2006-06-08 14:26:19	500014140	1.977	35	1.977	1.977	1.977	1.977	1	1	1	1	1	0	0	1.951	1.951	5.6719	0	PROCESSED	57534.60375	2016-05-26 14:29:24	54267	2007-06-16 00:00:00	54052.5450231482	2006-11-13 13:04:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014140/	Quick Look
85	MBM12	44.0042	19.487	43.295962	19.285573	47.250431	2.610049	159.18888296	-34.46916863	253.4644	53769.9600578704	2006-02-03 23:02:29	53772.6460416667	2006-02-06 15:30:18	500015010	102.9371	100	102.9371	102.9371	102.9371	102.9371	2	2	2	2	1	0	0	93.6709	93.6709	232.0499	1	PROCESSED	57532.9850694444	2016-05-24 23:38:30	54247	2007-05-27 00:00:00	54041.1327662037	2006-11-02 03:11:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001059	Suzaku can potentially determine the time since the nearby supernova that created (or reheated) the Local Hot Bubble (LHB) by measuring the ratio of the O VII/O VIII lines emitted by the LHB. The LHB temperature is ~10^6 K, and in equilibrium we would expect no O VIII emission. However, the LHB is almost certainly not in equilibrium, and it is quite possible that significant O^{+7} is still recombining (and emitting O VIII) following its creation in the most recent local supernova 2-4 Myr ago. We propose to measure these lines from the LHB using the nearby molecular cloud MBM12 as a curtain to shadow more distant emission. Even if O VIII is not detected, the O VII measurement will be the first unambiguous measurement of a line from the LHB.	GALACTIC DIFFUSE EMISSION	5	A	RANDALL SMITH		JAP	0	SWG	DATING THE LOCAL HOT BUBBLE WITH SUZAKU	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500015010/	Quick Look
86	CYGNUS LOOP NE4	313.5005	32.369	312.987812	32.178281	329.006135	47.302265	75.72495347	-7.98937114	221.2023	53704.2368287037	2005-11-30 05:41:02	53704.7661342593	2005-11-30 18:23:14	500023010	25.0049	20	25.0049	25.2689	25.0067	25.0689	2	2	2	2	1	0	0	25.1249	25.1249	45.726	1	PROCESSED	57532.3510763889	2016-05-24 08:25:33	54247	2007-05-27 00:00:00	54038.67625	2006-10-30 16:13:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001093	We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	0	SWG	CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500023010/	Quick Look
87	VICINITY OF LMC X-3	83.4844	-63.8863	83.408578	-63.918105	41.435206	-86.187449	273.3865557	-32.64248934	284.6189	53811.6008333333	2006-03-17 14:25:12	53813.9168055556	2006-03-19 22:00:12	500031010	82.0185	80	82.0265	82.0185	82.0265	82.0265	2	2	2	2	1	0	0	74.6148	74.6148	200.0639	2	PROCESSED	57533.2849537037	2016-05-25 06:50:20	54247	2007-05-27 00:00:00	54056.4806828704	2006-11-17 11:32:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000043	We propose to observe the vicnity of LMC X-3 for 80 ks. We expectt to determine the OVII and OVIII emission line intensities within 20% errors. Combining these results with the OVII and OVIII absorption lines observed in the energy spectra of LMC X-3 with Chandra LETG-HRC, we can determine the geometrocal extent od the hot gas along the line-of-sight direction. This will answer the long-unanswered question; from where the high lattitude OVII/OVIII emissions come ?	GALACTIC DIFFUSE EMISSION	5	A	SWG		JAP	0	SWG	VICINITY OF LMC X-3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500031010/	Quick Look
88	IC 443	94.2975	22.7757	93.54026	22.794725	93.963954	-0.606095	188.8694635	3.11574616	274.0004	54165.4446643518	2007-03-06 10:40:19	54166.5154398148	2007-03-07 12:22:14	501006010	42.0113	40	42.0113	42.0129	0	42.0209	2	2	0	2	1	0	0	34.6934	34.6934	92.5099	2	PROCESSED	57537.6197337963	2016-05-29 14:52:25	54736	2008-09-27 00:00:00	54174.6613541667	2007-03-15 15:52:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010040	IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution.	GALACTIC DIFFUSE EMISSION	5	B	MASANOBU OZAKI		JAP	1	AO1	UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501006010/	Quick Look
89	CYGNUS_LOOP_P1	313.519	31.9657	313.004288	31.774919	328.788742	46.92673	75.41990185	-8.25713566	240	54417.6059259259	2007-11-13 14:32:32	54418.0904976852	2007-11-14 02:10:19	501012010	16.7385	10	16.7385	16.7489	0	16.7425	2	2	0	2	1	0	0	15.7758	15.7758	41.86	1	PROCESSED	57540.5110648148	2016-06-01 12:15:56	54798	2008-11-28 00:00:00	54430.2159375	2007-11-26 05:10:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501012010/	Quick Look
90	CYGNUS_LOOP_P4	312.8083	31.361	312.292075	31.17275	327.627486	46.612051	74.56035476	-8.16867105	239.9997	54418.9382291667	2007-11-14 22:31:03	54419.3196643518	2007-11-15 07:40:19	501015010	18.279	15	18.287	18.279	0	18.287	1	1	0	1	1	0	0	14.286	14.286	32.9439	0	PROCESSED	57540.5253935185	2016-06-01 12:36:34	54798	2008-11-28 00:00:00	54430.2398726852	2007-11-26 05:45:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501015010/	Quick Look
91	CYGNUS_LOOP_P5	312.5567	31.1701	312.040041	30.982753	327.230821	46.520779	74.2739834	-8.12038976	239.9995	54419.3201388889	2007-11-15 07:41:00	54420.0627777778	2007-11-16 01:30:24	501016010	28.4062	22	28.4062	28.4062	0	28.4062	2	2	0	2	1	0	0	25.37	25.37	64.1559	1	PROCESSED	57540.538900463	2016-06-01 12:56:01	54798	2008-11-28 00:00:00	54430.4318865741	2007-11-26 10:21:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501016010/	Quick Look
92	CYGNUS_LOOP_P6	312.3057	30.9823	311.788615	30.795857	326.837045	46.431585	73.99029438	-8.06939848	240.0003	54415.3923032407	2007-11-11 09:24:55	54416.1668287037	2007-11-12 04:00:14	501017010	28.7049	22	28.7049	28.7049	0	28.7049	1	1	0	1	1	0	0	26.8878	26.8878	66.9119	0	PROCESSED	57540.490474537	2016-06-01 11:46:17	54798	2008-11-28 00:00:00	54430.18875	2007-11-26 04:31:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501017010/	Quick Look
93	CYGNUS_LOOP_P16	312.737	30.4592	312.216541	30.271212	327.037451	45.805605	73.81069789	-8.68546284	61.9998	53877.1905439815	2006-05-22 04:34:23	53877.7605671296	2006-05-22 18:15:13	501033010	23.3375	22	23.3695	23.3375	23.3695	23.3695	2	2	2	2	1	0	0	20.1184	20.1184	49.2439	2	PROCESSED	57534.3873611111	2016-05-26 09:17:48	54398	2007-10-25 00:00:00	53926.8416319445	2006-07-10 20:11:57	3.0.22.43	6	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501033010/	Quick Look
94	GC_SGR_B_NORTH	266.6955	-28.3829	265.90467	-28.36493	267.072555	-4.975375	0.60514127	0.06995468	271.4417	54002.2105555556	2006-09-24 05:03:12	54003.2919444444	2006-09-25 07:00:24	501040020	44.8295	38	44.8455	44.8295	44.8375	44.8535	2	2	2	2	1	0	0	39.9705	39.9705	93.4319	1	PROCESSED	57535.678125	2016-05-27 16:16:30	54744	2008-10-05 00:00:00	54021.2868055556	2006-10-13 06:53:00	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010060	We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	1	AO1	OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501040020/	Quick Look
95	HESS J1614-518	243.5851	-51.743	242.630135	-51.617031	251.446035	-29.987821	331.574855	-0.5276897	283.402	53993.6672222222	2006-09-15 16:00:48	53994.4571064815	2006-09-16 10:58:14	501042010	40.1777	50	40.1857	40.1777	40.1857	40.1857	2	2	2	2	1	0	0	43.5607	43.5607	68.2279	0	PROCESSED	57535.5776967593	2016-05-27 13:51:53	54526	2008-03-01 00:00:00	54020.8545833333	2006-10-12 20:30:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010073	We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	1	AO1	SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501042010/	Quick Look
96	HESS J1614-518 BG	242.0174	-52.4329	241.059171	-52.300176	250.522759	-30.865237	330.3996927	-0.37656553	291.2192	53994.4597569444	2006-09-16 11:02:03	53995.3015509259	2006-09-17 07:14:14	501043010	43.5554	50	43.5634	43.5634	43.5554	43.5634	1	1	1	1	1	0	0	50.5922	50.5922	72.7039	1	PROCESSED	57535.5823726852	2016-05-27 13:58:37	54526	2008-03-01 00:00:00	54020.8662268518	2006-10-12 20:47:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010073	We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	1	AO1	SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501043010/	Quick Look
97	GALACTIC CENTER GC3	265.5781	-29.4684	264.780645	-29.444998	266.119721	-6.086772	359.1684549	0.33584661	108.8001	54170.7951273148	2007-03-11 19:04:59	54171.3397453704	2007-03-12 08:09:14	501048010	27.4546	25	27.4786	27.4546	0	27.4786	1	1	0	1	1	0	0	24.0548	24.0548	47.0479	1	PROCESSED	57537.6483333333	2016-05-29 15:33:36	54736	2008-09-27 00:00:00	54182.2788425926	2007-03-23 06:41:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501048010/	Quick Look
98	GALACTIC CENTER	265.9089	-29.649	265.11021	-29.627197	266.414403	-6.258746	359.16615355	-0.00387238	269	54017.0975115741	2006-10-09 02:20:25	54017.5690277778	2006-10-09 13:39:24	501050010	22.0477	20	22.0477	22.0477	22.0477	22.0477	1	1	1	1	1	0	0	18.6256	18.6256	40.7359	0	PROCESSED	57535.8013194445	2016-05-27 19:13:54	54735	2008-09-26 00:00:00	54053.4127777778	2006-11-14 09:54:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501050010/	Quick Look
99	GALACTIC CENTER	265.2994	-30.4982	264.495374	-30.473432	265.90984	-7.123709	358.16648703	-0.00302139	269.0003	54018.8881828704	2006-10-10 21:18:59	54019.4209953704	2006-10-11 10:06:14	501053010	21.9086	20	21.9086	21.9321	21.9166	21.9166	1	1	1	1	1	0	0	19.948	19.948	46.0319	0	PROCESSED	57535.8190393518	2016-05-27 19:39:25	54735	2008-09-26 00:00:00	54053.5019675926	2006-11-14 12:02:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501053010/	Quick Look
100	GC SGR D EAST	267.2856	-27.6502	266.49923	-27.635104	267.579665	-4.231943	1.50163715	0.00269695	108.7997	54176.2132407407	2007-03-17 05:07:04	54177.8737731482	2007-03-18 20:58:14	501060010	64.7953	63	64.7953	64.8267	0	64.8113	2	2	0	2	1	0	0	54.6297	54.6297	143.4659	1	PROCESSED	57537.7151851852	2016-05-29 17:09:52	54736	2008-09-27 00:00:00	54185.4429050926	2007-03-26 10:37:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501060010/	Quick Look
101	RXJ1713-3946	258.5524	-39.4291	257.687827	-39.37177	260.79719	-16.352329	347.6770378	-0.38034705	267.9999	53997.5713773148	2006-09-19 13:42:47	53997.9140509259	2006-09-19 21:56:14	501069010	18.375	20	18.375	18.375	18.375	18.375	1	1	1	1	1	0	0	14.2767	14.2767	29.5999	0	PROCESSED	57535.6332060185	2016-05-27 15:11:49	54526	2008-03-01 00:00:00	54021.1502546296	2006-10-13 03:36:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501069010/	Quick Look
102	RXJ1713-3946	258.9408	-39.7267	258.073523	-39.671212	261.133474	-16.624716	347.60984156	-0.7970823	268.0009	54013.3138541667	2006-10-05 07:31:57	54013.877974537	2006-10-05 21:04:17	501072010	19.9817	20	19.9817	19.9817	19.9817	19.9817	2	2	2	2	1	0	0	16.2997	16.2997	48.718	1	PROCESSED	57535.7676736111	2016-05-27 18:25:27	54526	2008-03-01 00:00:00	54021.6599652778	2006-10-13 15:50:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501072010/	Quick Look
103	G156.2+5.7NW	74.223	52.4174	73.2357	52.339427	79.010107	29.577951	155.48379099	5.80912082	273.883	54147.6530902778	2007-02-16 15:40:27	54148.7558333333	2007-02-17 18:08:24	501075010	50.5468	50	50.5468	50.5468	0	50.5468	2	2	0	2	1	0	0	46.1958	46.1958	95.2599	0	PROCESSED	57537.3885763889	2016-05-29 09:19:33	54695	2008-08-17 00:00:00	54153.2775	2007-02-22 06:39:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011235	G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target.	GALACTIC DIFFUSE EMISSION	5	C	ROBERT PETRE		USA	1	AO1	A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501075010/	Quick Look
104	SNR G93.3+6.9 CENTER	312.9805	55.373	312.634427	55.183848	352.046818	66.979241	93.25121789	6.97467523	40.9208	53905.2215509259	2006-06-19 05:19:02	53905.6480787037	2006-06-19 15:33:14	501079010	20.5372	20	20.5452	20.5452	20.5452	20.5372	2	2	2	2	1	0	0	20.008	20.008	36.8159	0	PROCESSED	57534.7200347222	2016-05-26 17:16:51	54401	2007-10-28 00:00:00	53926.792962963	2006-07-10 19:01:52	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501079010/	Quick Look
105	SNR G93.3+6.9 S1	313.1088	55.5284	312.76382	55.338789	352.457306	67.040407	93.41888838	7.01647125	40.6424	53905.6486458333	2006-06-19 15:34:03	53905.9696064815	2006-06-19 23:16:14	501080010	15.875	15	15.875	15.8902	15.891	15.883	1	1	1	1	1	0	0	12.7588	12.7588	27.7279	1	PROCESSED	57534.7111805556	2016-05-26 17:04:06	54401	2007-10-28 00:00:00	53926.199212963	2006-07-10 04:46:52	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501080010/	Quick Look
106	SNR G93.3+6.9 S4	312.7524	55.2472	312.406034	55.058863	351.58456	66.978212	93.07038921	6.99620044	39.4008	53906.7271296296	2006-06-20 17:27:04	53907.0550347222	2006-06-21 01:19:15	501083010	15.3662	15	15.3662	15.3662	15.3662	15.3662	2	2	2	2	1	0	0	14.4694	14.4694	28.3279	1	PROCESSED	57534.7341550926	2016-05-26 17:37:11	54401	2007-10-28 00:00:00	53926.117662037	2006-07-10 02:49:26	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501083010/	Quick Look
107	HESS J1718-385	259.5512	-38.6075	258.69231	-38.554942	261.534502	-15.472357	348.79652534	-0.53531102	91.2393	54154.3587731482	2007-02-23 08:36:38	54154.7773611111	2007-02-23 18:39:24	501105010	20.744	19	20.744	20.744	0	20.744	1	1	0	1	1	0	0	15.8365	15.8365	36.1519	0	PROCESSED	57537.4491435185	2016-05-29 10:46:46	54527	2008-03-02 00:00:00	54158.2865740741	2007-02-27 06:52:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012044	HESS J1718-385 is a newly discovered TeV gamma-ray source, with an unusually hard energy spectrum, which lies in close proximity to an energetic pulsar. It is likely that this object belongs to the class of offset pulsar wind nebula (PWN), accelerating electrons and positrons up to ~100 TeV. So far no sensitive X-ray observations of this region have taken place. The synchrotron spectrum of the nebula is predicted to peak in the energy range of the Suzaku HXD. The unprecedented high energy sensitivity of this instrument is required to study the highest energy particles accelerated in this object. Spectral measurements by Suzaku would confirm the inverse-Compton origin of the VHE gamma-rays and place tight constraints on the maximum energy of accelerated electrons.	GALACTIC DIFFUSE EMISSION	5	A	JAMES HINTON		EUR	1	AO1	PROBING THE LIMITS OF PARTICLE ACCELERATION IN A NEW HARD SPECTRUM TEV GAMMA-RAY SOURCE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501105010/	Quick Look
108	G156.2+5.7 CENTER	74.723	51.7342	73.743251	51.658579	79.264036	28.862327	156.21466687	5.62934315	273.4473	54148.7568171296	2007-02-17 18:09:49	54149.9169444444	2007-02-18 22:00:24	501106010	51.2142	50	51.2222	51.2302	0	51.2142	1	1	0	1	1	0	0	46.482	46.482	100.1999	0	PROCESSED	57537.3992824074	2016-05-29 09:34:58	54695	2008-08-17 00:00:00	54158.4264351852	2007-02-27 10:14:04	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	013079	Recent observations revealed that about 10 shell-like supernova remnants (SNRs) exhibit power-law X-ray spectra with no emission line which are considered to be synchrotron radiation from high-energy electrons (larger than 1 TeV). However, all those samples are young SNRs (ages about 300-2000 yr). G156.2+5.7 is an old SNR (age about 10^4 year), but emits hard X-rays in addition to usual thin thermal emission (about 0.5 keV temperature). We propose a Suzaku observation on a center region of this SNR, where diffuse hard X-rays were detected with ASCA and XMM. Our primary objective is to determine whether or not the hard tail is synchrotron X-rays, and study cosmic-ray acceleration in this old SNR.	GALACTIC DIFFUSE EMISSION	5	B	MASARU UENO	ROBERT PETRE	JUS	1	AO1	REVEALING THE ORIGIN OF HARD X-RAY EMISSION FROM AN OLD SNR, G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501106010/	Quick Look
109	VELA X (REGION A)	128.7666	-45.458	128.346603	-45.284447	153.579861	-60.62666	263.74862198	-2.99483781	337.7597	53927.7846990741	2006-07-11 18:49:58	53929.4703819444	2006-07-13 11:17:21	501107010	60.7735	60	60.7735	60.7735	60.7735	60.7735	2	2	2	2	1	0	0	54.1611	54.1611	145.6058	3	PROCESSED	57534.9641203704	2016-05-26 23:08:20	54401	2007-10-28 00:00:00	53942.4562037037	2006-07-26 10:56:56	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014211	The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band.	GALACTIC DIFFUSE EMISSION	5	B	OLEG KARGALTSEV	KOJI MORI	USJ	1	AO1	THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501107010/	Quick Look
110	VELA X (REGION C)	127.7806	-46.2716	127.370041	-46.101802	153.218075	-61.676794	263.99736145	-4.03006469	349.189	53933.9133796296	2006-07-17 21:55:16	53934.7730787037	2006-07-18 18:33:14	501108010	29.2028	30	29.2028	29.2028	29.2028	29.2028	2	2	2	2	1	0	0	25.5929	25.5929	74.248	1	PROCESSED	57534.9868055556	2016-05-26 23:41:00	54404	2007-10-31 00:00:00	53943.4988773148	2006-07-27 11:58:23	3.0.22.43	7	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014211	The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band.	GALACTIC DIFFUSE EMISSION	5	B	OLEG KARGALTSEV	KOJI MORI	USJ	1	AO1	THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501108010/	Quick Look
111	GC18	266.183	-28.6222	265.39077	-28.601742	266.626489	-5.225763	0.16630142	0.32982124	260.5302	54384.4819560185	2007-10-11 11:34:01	54384.9633564815	2007-10-11 23:07:14	502006010	22.6311	20	22.6311	22.6413	0	22.6351	2	2	0	2	1	0	0	21.6702	21.6702	41.5841	1	PROCESSED	57540.2503356482	2016-06-01 06:00:29	54771	2008-11-01 00:00:00	54402.6632291667	2007-10-29 15:55:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502006010/	Quick Look
112	GC21	267.484	-27.3686	266.699338	-27.354471	267.750913	-3.947195	1.83363899	-0.00346152	261.5433	54385.9113888889	2007-10-12 21:52:24	54386.3127199074	2007-10-13 07:30:19	502009010	20.8615	20	20.8615	20.8615	0	20.8615	2	2	0	2	1	0	0	19.6483	19.6483	34.6639	1	PROCESSED	57540.2599189815	2016-06-01 06:14:17	54771	2008-11-01 00:00:00	54402.5769444444	2007-10-29 13:50:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502009010/	Quick Look
113	GC22	266.3806	-28.337	265.590118	-28.317504	266.793387	-4.936169	0.50023196	0.3305092	262.5049	54386.3138888889	2007-10-13 07:32:00	54386.785	2007-10-13 18:50:24	502010010	21.6214	20	21.6214	21.6214	0	21.6214	2	2	0	2	1	0	0	21.1944	21.1944	40.662	1	PROCESSED	57540.2655439815	2016-06-01 06:22:23	54771	2008-11-01 00:00:00	54402.6900231482	2007-10-29 16:33:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502010010/	Quick Look
114	HESS J1745-303 3	266.0567	-30.2413	265.254155	-30.220204	266.559978	-6.847208	358.72882707	-0.42335991	69.0003	54533.6682523148	2008-03-08 16:02:17	54535.8752199074	2008-03-10 21:00:19	502018010	79.0162	67	79.0162	79.0402	0	79.0242	2	2	0	2	1	0	0	70.201	70.201	190.658	2	PROCESSED	57541.8566898148	2016-06-02 20:33:38	54919	2009-03-29 00:00:00	54550.3420601852	2008-03-25 08:12:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020023	A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku.	GALACTIC DIFFUSE EMISSION	5	B	RYO YAMAZAKI		JAP	2	AO2	SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502018010/	Quick Look
115	VELA JR P7	133.7759	-45.5828	133.340558	-45.390922	159.660843	-58.904253	266.02998701	-0.32446592	347.0033	54286.9870023148	2007-07-05 23:41:17	54287.3023032407	2007-07-06 07:15:19	502029010	14.5838	10	14.5838	14.5838	0	14.5838	2	2	0	2	1	0	0	12.605	12.605	27.2399	0	PROCESSED	57539.1100810185	2016-05-31 02:38:31	54696	2008-08-18 00:00:00	54328.4686111111	2007-08-16 11:14:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502029010/	Quick Look
116	VELA JR P10	132.9993	-45.7656	132.567919	-45.576468	158.955645	-59.347984	265.8217159	-0.85784968	347.0018	54287.9522337963	2007-07-06 22:51:13	54288.2308564815	2007-07-07 05:32:26	502032010	13.04	10	13.048	13.04	0	13.056	2	2	0	2	1	0	0	10.6988	10.6988	24.0679	0	PROCESSED	57539.1146527778	2016-05-31 02:45:06	54703	2008-08-25 00:00:00	54333.4328240741	2007-08-21 10:23:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502032010/	Quick Look
117	VELA JR P14	131.9312	-46.3861	131.508056	-46.200795	158.369308	-60.268301	265.83284327	-1.824218	347.0017	54290.4416087963	2007-07-09 10:35:55	54290.675150463	2007-07-09 16:12:13	502036010	11.034	10	11.034	11.042	0	11.042	1	1	0	1	1	0	0	11.1391	11.1391	20.1679	0	PROCESSED	57539.1311226852	2016-05-31 03:08:49	54696	2008-08-18 00:00:00	54328.4740277778	2007-08-16 11:22:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502036010/	Quick Look
118	VELA JR P15	132.3334	-46.3288	131.908455	-46.142044	158.77835	-60.071	265.96324441	-1.57253381	347.0016	54291.1946064815	2007-07-10 04:40:14	54291.46	2007-07-10 11:02:24	502037010	8.876	10	8.876	8.876	0	8.876	2	2	0	2	1	0	0	7.3411	7.3411	22.9121	1	PROCESSED	57539.1396990741	2016-05-31 03:21:10	54696	2008-08-18 00:00:00	54328.472962963	2007-08-16 11:21:04	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502037010/	Quick Look
119	47 TUCANAE	6.2112	-71.9961	5.659821	-72.273106	311.457534	-62.358991	305.8317488	-44.9821189	65.5967	54261.1765162037	2007-06-10 04:14:11	54263.5404976852	2007-06-12 12:58:19	502048010	132.1052	133	132.1452	132.1052	0	132.1372	2	2	0	2	1	0	0	132.9042	132.9042	204.2319	1	PROCESSED	57538.9491666667	2016-05-30 22:46:48	54745	2008-10-06 00:00:00	54271.5258796296	2007-06-20 12:37:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020066	We propose a 100 ks observation of the globular cluster 47 Tuc. An extended (~2') hard x-ray emission, presumably of non-thermal origin, was detected with Chandra from a position ~6' toward north east of its center. However, the Chandra ACIS spectrum does not allow us to determine with confidence whether it is a non-thermal emission or a high temperature thermal source. Utilizing the high sensitivity of the XIS, we try to distinguish between these two cases. If confirmed, the result may provide valuable information on particle acceleration in non-relativistic shocks, with potential relations the galactic-ridge x-ray emission. We perform a single pointing observation placing the center of the diffuse emission onto XIS nominal position.	GALACTIC DIFFUSE EMISSION	5	B	TAKAYUKI YUASA		JAP	2	AO2	OBSERVATIONAL INVESTIGATION OF PARTICLE ACCELERATION IN A GLOBULAR CLUSTER SHOCK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502048010/	Quick Look
120	M17 EAST BKG	275.6441	-15.5803	274.925967	-15.60595	275.476675	7.75309	15.81995827	-0.84785909	271.9998	54380.0947800926	2007-10-07 02:16:29	54381.7571064815	2007-10-08 18:10:14	502053010	71.494	67	71.494	71.5085	0	71.502	2	2	0	2	1	0	0	62.5549	62.5549	143.61	1	PROCESSED	57540.2032175926	2016-06-01 04:52:38	54771	2008-11-01 00:00:00	54403.2344791667	2007-10-30 05:37:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020085	We continue our XIS study of the soft extended X-ray emission in M17. The first study conducted in a region close to the OB association brought a detailed surface brightness distribution and the highest S/N ratio spectrum of the diffuse emission. In this proposed study, we move our eyes to the west to observe another bright emission outside of the previously studied regions. DSS and ROSAT all-sky survey images suggest that this is a shocked region, in which OB stellar winds impinge upon ISM. We aim to obtain the surface brightness map of this region and measure the plasma temperature difference in and out of the possible shocked region.	GALACTIC DIFFUSE EMISSION	5	A	MASAHIRO TSUJIMOTO		JAP	2	AO2	FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS -	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502053010/	Quick Look
121	GALACTIC BULGE	268.3774	-29.9651	267.576244	-29.955267	268.575567	-6.53206	359.99980668	-2.0020922	279.4328	54372.0700347222	2007-09-29 01:40:51	54375.590462963	2007-10-02 14:10:16	502059010	136.824	133	136.824	136.824	0	136.824	2	2	0	2	1	0	0	110.5156	110.5156	304.1306	2	PROCESSED	57540.2260185185	2016-06-01 05:25:28	54770	2008-10-31 00:00:00	54402.653275463	2007-10-29 15:40:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020118	We propose a 100 ks observation on the Galactic Bulge (b=-2.0) with Suzaku. The origin of thermal diffuse X-ray emission will be for the first time clarified with a fine spectroscopy with Suzaku XIS, especially from the Fe-K line analysis. The non-thermal emission from the Galactic Bulge will be also investigated with HXD-PIN.	GALACTIC DIFFUSE EMISSION	5	A	MOTOHIDE KOKUBUN		JAP	2	AO2	INVESTIGATION ON THE GALACTIC BULGE DIFFUSE X-RAY EMISSION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502059010/	Quick Look
122	COMET_8P_TUTTLE-P1-9	28.3593	5.9969	27.705197	5.751157	28.487543	-5.283181	149.56477648	-53.63811023	248.4989	54471.0491666667	2008-01-06 01:10:48	54471.1154050926	2008-01-06 02:46:11	502062090	3.2186	3.2	3.2186	3.2186	0	3.2186	1	1	0	1	1	0	0	2.439	2.439	5.664	0	PROCESSED	57541.0088425926	2016-06-02 00:12:44	54908	2009-03-18 00:00:00	54542.2348611111	2008-03-17 05:38:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062090/	Quick Look
123	COMET_8P_TUTTLE-P1-11	28.4619	5.5053	27.808889	5.259792	28.409931	-5.779338	150.05998726	-54.04643055	248.5015	54471.1825	2008-01-06 04:22:48	54471.2487384259	2008-01-06 05:58:11	502062110	3.219	3.2	3.219	3.219	0	3.219	1	1	0	1	1	0	0	2.0356	2.0356	5.688	0	PROCESSED	57541.2689699074	2016-06-02 06:27:19	54908	2009-03-18 00:00:00	54542.2871990741	2008-03-17 06:53:34	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062110/	Quick Look
124	COMET_8P_TUTTLE-P1-12	28.5143	5.2526	27.861852	5.007213	28.369731	-6.034275	150.31791041	-54.25562458	248.4993	54471.2491666667	2008-01-06 05:58:48	54471.3154050926	2008-01-06 07:34:11	502062120	3.2196	3.2	3.2196	3.2196	0	3.2196	1	1	0	1	1	0	0	2.162	2.162	5.696	0	PROCESSED	57541.268587963	2016-06-02 06:26:46	54908	2009-03-18 00:00:00	54542.261400463	2008-03-17 06:16:25	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062120/	Quick Look
125	COMET_8P_TUTTLE-P2_03	39.7649	-35.9737	39.253357	-36.188553	21.195094	-48.151161	240.80897167	-65.5250468	257.7596	54490.2964351852	2008-01-25 07:06:52	54490.4293287037	2008-01-25 10:18:14	502063030	6.0389	6	6.0549	6.0389	0	6.0549	2	2	0	2	1	0	0	6.6011	6.6011	11.4639	0	PROCESSED	57541.3810532407	2016-06-02 09:08:43	54912	2009-03-22 00:00:00	54546.1040046296	2008-03-21 02:29:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063030/	Quick Look
126	COMET_8P_TUTTLE-P2_04	39.8249	-36.1145	39.31419	-36.329166	21.162848	-48.298537	241.11100541	-65.44459708	257.8515	54490.4297106482	2008-01-25 10:18:47	54490.562662037	2008-01-25 13:30:14	502063040	6.6876	6.7	6.6876	6.7191	0	6.6876	1	1	0	1	1	0	0	7.3887	7.3887	11.4799	0	PROCESSED	57541.3859375	2016-06-02 09:15:45	54912	2009-03-22 00:00:00	54546.1129513889	2008-03-21 02:42:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063040/	Quick Look
127	COMET_8P_TUTTLE-P2_05	39.8852	-36.2545	39.375324	-36.468978	21.131041	-48.445251	241.40935004	-65.36366996	257.9439	54490.5630439815	2008-01-25 13:30:47	54490.6959953704	2008-01-25 16:42:14	502063050	6.6974	6.7	6.6976	6.6976	0	6.6974	1	1	0	1	1	0	0	6.1619	6.1619	11.4799	0	PROCESSED	57541.3887847222	2016-06-02 09:19:51	54912	2009-03-22 00:00:00	54546.126712963	2008-03-21 03:02:28	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063050/	Quick Look
128	COMET_8P_TUTTLE-P2_10	40.1849	-36.9375	39.679167	-37.15104	20.975454	-49.162155	242.83840601	-64.95862507	253.4045	54491.2297106482	2008-01-26 05:30:47	54491.362662037	2008-01-26 08:42:14	502063100	5.7304	5	5.7384	5.7384	0	5.7304	2	2	0	2	1	0	0	6.2091	6.2091	11.4739	0	PROCESSED	57541.4028472222	2016-06-02 09:40:06	54912	2009-03-22 00:00:00	54546.1949884259	2008-03-21 04:40:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063100/	Quick Look
129	COMET_8P_TUTTLE-P2_12	40.3045	-37.2045	39.80042	-37.417664	20.914316	-49.442898	243.38522043	-64.79583615	253.5926	54491.4963773148	2008-01-26 11:54:47	54491.6293287037	2008-01-26 15:06:14	502063120	6.6082	6.7	6.6082	6.6082	0	6.6242	1	1	0	1	1	0	0	6.4698	6.4698	11.4799	0	PROCESSED	57541.4099884259	2016-06-02 09:50:23	54912	2009-03-22 00:00:00	54546.2619675926	2008-03-21 06:17:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063120/	Quick Look
130	COMET_8P_TUTTLE-P2_14	40.423	-37.4668	39.920562	-37.679591	20.853678	-49.718838	243.91615364	-64.63380941	253.7796	54491.7630439815	2008-01-26 18:18:47	54491.8959953704	2008-01-26 21:30:14	502063140	6.5627	6.7	6.5627	6.5867	0	6.5627	1	1	0	1	1	0	0	3.833	3.833	11.4799	0	PROCESSED	57541.4134143518	2016-06-02 09:55:19	54912	2009-03-22 00:00:00	54546.2568518518	2008-03-21 06:09:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063140/	Quick Look
131	COMET_8P_TUTTLE-P2_15	40.4836	-37.5961	39.981983	-37.8087	20.825541	-49.855587	244.17467378	-64.55180166	253.8725	54491.8963773148	2008-01-26 21:30:47	54492.0293287037	2008-01-27 00:42:14	502063150	3.4717	4	3.4797	3.4717	0	3.4877	1	1	0	1	1	0	0	2.3461	2.3461	11.4799	1	PROCESSED	57541.4238657407	2016-06-02 10:10:22	54912	2009-03-22 00:00:00	54546.2153587963	2008-03-21 05:10:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063150/	Quick Look
132	G332.5-5.6 CENTER	250.7335	-54.5135	249.725841	-54.419293	256.94436	-31.940577	332.53119736	-5.54004522	262.5079	54330.694224537	2007-08-18 16:39:41	54331.8731944444	2007-08-19 20:57:24	502066010	70.1488	80	70.1488	70.1488	0	70.1568	1	1	0	1	1	0	0	71.4907	71.4907	101.8399	0	PROCESSED	57539.62875	2016-05-31 15:05:24	54721	2008-09-12 00:00:00	54354.4910300926	2007-09-11 11:47:05	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021216	We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova.	GALACTIC DIFFUSE EMISSION	5	B	STEPHEN REYNOLDS		USA	2	AO2	G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502066010/	Quick Look
133	KEPLER	262.6698	-21.4886	261.920525	-21.451271	263.169114	1.778808	4.51918955	6.82146946	98.2145	54514.1665393518	2008-02-18 03:59:49	54516.9793287037	2008-02-20 23:30:14	502078010	116.9636	100	116.9636	116.9636	0	116.9636	2	2	0	2	1	0	0	98.9551	98.9551	242.9956	3	PROCESSED	57541.7751388889	2016-06-02 18:36:12	54894	2009-03-04 00:00:00	54525.6176851852	2008-02-29 14:49:28	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	023074	We propose to observe the Kepler's SNR in which evidence of particle acceleration will be found. Aim of the observation is to determine power-law contribution in the hard-tail spectrum above 10 keV with HXD-PIN. If we also find the Fe-Kb and Ni-K emission lines with XIS which have not observed in any previous missions, temperature and nt parameter of a NEI model will be fixed. The determination will help to distinguish the power-law component from the thermal one. We also memtioned that the amount of Fe and Ni will be a good estimator to determine the type of Kepler's SNR.	GALACTIC DIFFUSE EMISSION	5	B	TORU TAMAGAWA	Sangwook Park	JUS	2	AO2	SEARCH FOR EVIDENCE OF COSMIC-RAY ACCELERATION IN THE KEPLER'S SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502078010/	Quick Look
134	ANTICENTER2	12.9862	62.9112	12.227424	62.639587	45.279185	50.910305	122.98962226	0.03950805	69.9598	54679.0120717593	2008-08-01 00:17:23	54680.8411921296	2008-08-02 20:11:19	503006010	86.1101	80	86.123	86.123	0	86.1101	2	2	0	2	1	0	0	106.785	106.785	158.0198	1	PROCESSED	57543.2173726852	2016-06-04 05:13:01	55070	2009-08-27 00:00:00	54693.3237847222	2008-08-15 07:46:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030020	We propose to observe diffuse radiation from the Galactic plane in the general direction of the anticenter. The ROSAT 3/4 keV band all sky map does not show significant dip in intensity at galactic plane, where the CXB component is totally absorbed by galactic absorption. Thus unknown emission must be compensating the CXB component in this energy band. Our AO-2 observation of a general direction of the anticenter direction gives a clear clue to understand the origin of the mysterious emission. We propose to make additional observation in order to confirm the emission component detected in the AO-2 observation generally exist in the galactic plane.	GALACTIC DIFFUSE EMISSION	5	B	KENSUKE MASUI		JAP	3	AO3	SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503006010/	Quick Look
135	GC_LARGEPROJECT2	266.7785	-29.1292	265.982946	-29.111621	267.162656	-5.719811	0.00479668	-0.37932142	260.8763	54712.9538078704	2008-09-03 22:53:29	54714.2891087963	2008-09-05 06:56:19	503008010	53.6388	50	53.6548	53.6388	0	53.6548	2	2	0	2	1	0	0	42.8111	42.8111	115.3338	0	PROCESSED	57543.7762615741	2016-06-04 18:37:49	54557	2008-04-01 00:00:00	54780.4880092593	2008-11-10 11:42:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503008010/	Quick Look
136	GC_LARGEPROJECT3	266.4525	-29.3384	265.655678	-29.319237	266.881748	-5.935661	359.67825031	-0.24492188	260.8779	54714.2896759259	2008-09-05 06:57:08	54715.6634722222	2008-09-06 15:55:24	503009010	52.3975	50	52.4055	52.3975	0	52.4114	2	2	0	2	1	0	0	40.2691	40.2691	118.6778	2	PROCESSED	57543.769375	2016-06-04 18:27:54	54557	2008-04-01 00:00:00	54780.6767476852	2008-11-10 16:14:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503009010/	Quick Look
137	GC_LARGEPROJECT5	265.9469	-29.8331	265.147019	-29.811478	266.45285	-6.44183	359.02671432	-0.12852462	265.43	54717.3806597222	2008-09-08 09:08:09	54718.8981365741	2008-09-09 21:33:19	503011010	57.6334	50	57.6334	57.6334	0	57.6334	2	2	0	2	1	0	0	40.1555	40.1555	131.0998	1	PROCESSED	57543.8408449074	2016-06-04 20:10:49	54557	2008-04-01 00:00:00	54780.6683912037	2008-11-10 16:02:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503011010/	Quick Look
138	GC_LARGEPROJECT9	265.0297	-30.9626	264.222709	-30.936519	265.692051	-7.595667	357.64981902	-0.05267713	269.1132	54728.3146412037	2008-09-19 07:33:05	54729.4140393518	2008-09-20 09:56:13	503015010	56.7716	50	56.7796	56.7716	0	56.7876	2	2	0	2	1	0	0	52.8454	52.8454	94.9759	0	PROCESSED	57543.8851041667	2016-06-04 21:14:33	54557	2008-04-01 00:00:00	54780.4933564815	2008-11-10 11:50:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503015010/	Quick Look
139	GC_LARGEPROJECT12	264.5606	-31.5967	263.749555	-31.56834	265.310874	-8.24393	356.89961278	-0.05143068	268.4538	54742.7536226852	2008-10-03 18:05:13	54743.154375	2008-10-04 03:42:18	503018020	12.2466	10	12.2466	12.2466	0	12.2466	2	2	0	2	1	0	0	10.232	10.232	34.6179	1	PROCESSED	57544.0096527778	2016-06-05 00:13:54	54557	2008-04-01 00:00:00	54780.5624652778	2008-11-10 13:29:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503018020/	Quick Look
140	HESS J1825-137	276.5024	-13.9965	275.79256	-14.02632	276.383198	9.300131	17.60816681	-0.84042551	271.0002	54754.9096064815	2008-10-15 21:49:50	54756.458599537	2008-10-17 11:00:23	503028010	57.2104	50	57.2104	57.2104	0	57.2104	2	2	0	2	1	0	0	51.5485	51.5485	133.7938	1	PROCESSED	57544.1955324074	2016-06-05 04:41:34	55148	2009-11-13 00:00:00	54780.7053703704	2008-11-10 16:55:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030044	The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons.	GALACTIC DIFFUSE EMISSION	5	B	TAKAAKI TANAKA		JAP	3	AO3	MAPPING OBSERVATIONS OF HESS J1825-137	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503028010/	Quick Look
141	VELA JR P24	132.0303	-46.6729	131.609003	-46.487232	158.79782	-60.473277	266.0989339	-1.95139979	347.001	54652.7719328704	2008-07-05 18:31:35	54653.1668865741	2008-07-06 04:00:19	503036010	12.3735	10	12.3735	12.3735	0	12.3735	2	2	0	2	1	0	0	12.2548	12.2548	34.12	1	PROCESSED	57542.9791203704	2016-06-03 23:29:56	55048	2009-08-05 00:00:00	54679.3185763889	2008-08-01 07:38:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503036010/	Quick Look
142	VELA JR P28	133.7109	-46.6037	133.283226	-46.412037	160.667114	-59.788002	266.78076878	-1.01777641	347.0004	54654.1674537037	2008-07-07 04:01:08	54654.4259143518	2008-07-07 10:13:19	503040010	13.093	10	13.101	13.093	0	13.101	1	1	0	1	1	0	0	12.054	12.054	22.296	0	PROCESSED	57542.9904282407	2016-06-03 23:46:13	55048	2009-08-05 00:00:00	54679.3674421296	2008-08-01 08:49:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503040010/	Quick Look
143	VELA JR P29	134.0711	-46.43	133.640871	-46.237075	160.890422	-59.507166	266.80859879	-0.71638658	347	54654.4264814815	2008-07-07 10:14:08	54654.7203703704	2008-07-07 17:17:20	503041010	11.3685	10	11.3802	11.3685	0	11.3802	1	1	0	1	1	0	0	8.2225	8.2225	25.3679	0	PROCESSED	57542.9909606482	2016-06-03 23:46:59	55048	2009-08-05 00:00:00	54679.3958217593	2008-08-01 09:29:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503041010/	Quick Look
144	VELA JR P38	132.2003	-47.2308	131.782721	-47.04451	159.617188	-60.877835	266.60579829	-2.21244802	347.0003	54657.2423958333	2008-07-10 05:49:03	54657.5209953704	2008-07-10 12:30:14	503050010	14.0436	10	14.0436	14.0436	0	14.0596	1	1	0	1	1	0	0	11.426	11.426	24.0639	0	PROCESSED	57543.0197800926	2016-06-04 00:28:29	55037	2009-07-25 00:00:00	54670.2561111111	2008-07-23 06:08:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503050010/	Quick Look
145	RCW 38	134.7638	-47.5154	134.339139	-47.320051	162.870038	-60.148721	267.93999829	-1.06526988	109.8553	54788.5064351852	2008-11-18 12:09:16	54790.699525463	2008-11-20 16:47:19	503054010	81.5377	80	81.5495	81.5377	0	81.5415	2	2	0	2	1	0	0	60.9281	60.9281	189.4597	1	PROCESSED	57544.5092013889	2016-06-05 12:13:15	55171	2009-12-06 00:00:00	54811.741099537	2008-12-11 17:47:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030069	We propose to make Suzaku observation of HII region RCW 38 for 80 ksec in order to study non-thermal phenomena in a massive star-forming region. The region is thought to be a site of high energy particle acceleration by interaction of strong stellar wind from high-mass stars. The main purpose is to observe extended emission from RCW 38. The high resolution spectroscopy by XIS enables us to distinguish non-thermal emission from thermal component and to obtain properties of non-thermal component. In addition, HXD will detect non-thermal radiation from RCW 38.	GALACTIC DIFFUSE EMISSION	5	C	HIROKAZU ODAKA		JAP	3	AO3	SEARCH FOR NONTHERMAL RADIATION FROM MASSIVE STAR-FORMING REGION RCW 38	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503054010/	Quick Look
146	CYGNUS LOOP (P21)	313.196	32.4197	312.684204	32.23006	328.688835	47.452326	75.60030214	-7.75821821	61.9243	54619.9401967593	2008-06-02 22:33:53	54620.2975	2008-06-03 07:08:24	503057010	16.1703	15	16.1783	16.1703	0	16.1783	1	1	0	1	1	0	0	12.8903	12.8903	30.8639	0	PROCESSED	57542.700474537	2016-06-03 16:48:41	55003	2009-06-21 00:00:00	54636.2238078704	2008-06-19 05:22:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503057010/	Quick Look
147	RABBIT	214.6544	-60.9713	213.733054	-60.740946	236.398817	-43.82174	313.31134091	0.131367	105.7763	54876.850787037	2009-02-14 20:25:08	54877.5224421296	2009-02-15 12:32:19	503071010	21.274	20	21.282	21.274	0	21.29	1	1	0	1	1	0	0	18.0126	18.0126	57.984	0	PROCESSED	57545.5405439815	2016-06-06 12:58:23	55330	2010-05-14 00:00:00	54892.945162037	2009-03-02 22:41:02	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030076	K3/PSR J1420-6048 is one of the TeV gamma-ray pulsar wind nebulae detected by HESS, which are thought to be main particle accelerators to the Galactic Cosmic rays. It was also detected by EGRET and its X-ray spectrum is very hard. In order to reveal the radiation mechanism, we propose to observe the extended source for 50 ksec on HXD nominal position and contamination source for 20 ksec on XIS nominal position. The main purpose of this observation is to obtain the hard X-ray spectrum up to about 40 keV.	GALACTIC DIFFUSE EMISSION	5	C	TETSUICHI KISHISHITA		JAP	3	AO3	SUZAKU OBSERVATION OF TEV GAMMA-RAY PWN K3/PSR J1420-6048	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503071010/	Quick Look
148	HESS_J1809-193_N	272.4044	-19.3551	271.665869	-19.36499	272.264534	4.066746	11.02929838	0.07166066	112.001	54556.5874421296	2008-03-31 14:05:55	54557.6877662037	2008-04-01 16:30:23	503078010	51.5309	40	51.5389	51.5309	0	51.5461	2	2	0	2	1	0	0	34.8186	34.8186	95.0518	2	PROCESSED	57542.0290740741	2016-06-03 00:41:52	54950	2009-04-29 00:00:00	54571.3638888889	2008-04-15 08:44:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030126	A survey of the Galactic plane with H.E.S.S. has revealed the existance of several new very-high-energy (VHE) gamma-ray sources. As gamma rays are produced by interactions of relativistic particles, observing VHE emission reveals the acceleration sites of particles. Although it had been thought that such acceleration occur in the shock of SNR, it became clear that several VHE sources are pulsar wind nebulae (PWNe). This indicates that PWNe are also the acceleration sites of particles. HESS J1809-193 is a diffuse and a pulsar wind nebula candidate source, but details of the VHE emission mechanisms have been unclear yet. With the high sensitivity of XIS, we investigate spatial distribution of the spectrum around HESS J1809-193 and reveal its nature and the VHE emission mechanism.	GALACTIC DIFFUSE EMISSION	5	A	TAKAYASU ANADA		JAP	3	AO3	INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503078010/	Quick Look
149	VICINITY_OF_PKS_2155-1	329.2367	-30.5281	328.510685	-30.766467	320.669664	-16.905257	17.16872193	-51.86657338	55.8337	54585.7726736111	2008-04-29 18:32:39	54588.3542592593	2008-05-02 08:30:08	503082010	90.1812	80	90.1812	90.1812	0	90.1812	2	2	0	2	1	0	0	76.7921	76.7921	223.0237	4	PROCESSED	57542.4840277778	2016-06-03 11:37:00	54975	2009-05-24 00:00:00	54608.3373726852	2008-05-22 08:05:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030135	The highly ionized absorption lines of OVII, OVIII, and NeIX at z = 0 have been unambiguously detected toward the bright AGN PKS 2155-304 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII, OVIII and NeIX emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas.	GALACTIC DIFFUSE EMISSION	5	A	TOSHISHIGE HAGIHARA		JAP	3	AO3	STUDY OF WARM-HOT GAS TOWARD PKS 2155-304	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503082010/	Quick Look
150	B1920+10(1)	293.0298	10.9618	292.438521	10.854204	297.004439	32.268855	47.34140504	-3.87470613	252.2888	54772.350462963	2008-11-02 08:24:40	54774.137662037	2008-11-04 03:18:14	503090010	73.6033	70	73.6124	73.6033	0	73.6113	2	2	0	2	1	0	0	66.6682	66.6682	154.4039	3	PROCESSED	57544.3491550926	2016-06-05 08:22:47	55154	2009-11-19 00:00:00	54788.4472337963	2008-11-18 10:44:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031204	A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps.	GALACTIC DIFFUSE EMISSION	5	C	ZDENKA MISANOVIC		USA	3	AO3	STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503090010/	Quick Look
151	HESS J1023-575	155.5616	-57.7533	155.104313	-57.500238	195.408014	-59.737737	284.06754503	-0.45248582	284.3289	54617.1411458333	2008-05-31 03:23:15	54617.4515509259	2008-05-31 10:50:14	503092010	13.826	10	13.826	13.826	0	13.826	1	1	0	1	1	0	0	11.0573	11.0573	26.8159	1	PROCESSED	57542.6773842593	2016-06-03 16:15:26	54999	2009-06-17 00:00:00	54633.6961458333	2008-06-16 16:42:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031207	We propose to search the neighborhood of two extended TeV sources to determine if there are X-ray sources that are potentially pulsar wind nebulae powering them. One source is near the colliding wind binary RCW 49, which has been suggested as the accelerator, and would therefore represent a new source class if there is no other plausible accelerator in the neighborhood. The other is a very bright source first detected by MILAGRO in the Galactic plane, which has been shown to be a large, extended source by HESS. While there is in each case a proposed X-ray counterpart, only a part of each nebula has been imaged in hard X-rays, and so it is unknown if there are other, more plausible counterparts.	GALACTIC DIFFUSE EMISSION	5	B	MALLORY ROBERTS		USA	3	AO3	SEARCHING FOR X-RAY COUNTERPARTS OF TWO GALACTIC TEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503092010/	Quick Look
152	GCL2	264.8888	-28.9255	264.094972	-28.898771	265.497098	-5.564174	359.31035513	1.13376438	106.9569	54905.2789467593	2009-03-15 06:41:41	54905.9169444444	2009-03-15 22:00:24	503100010	25.7179	25	25.7179	25.7179	0	25.7179	1	1	0	1	1	0	0	24.146	24.146	55.1199	1	PROCESSED	57545.8116666667	2016-06-06 19:28:48	55329	2010-05-13 00:00:00	54917.3744675926	2009-03-27 08:59:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031234	We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity.	GALACTIC DIFFUSE EMISSION	5	B	FARHAD YUSEF-ZADEH		USA	3	AO3	A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503100010/	Quick Look
153	GCL3	265.2728	-28.8569	264.479303	-28.83203	265.832305	-5.484097	359.5469331	0.88519	106.9023	54906.6133912037	2009-03-16 14:43:17	54907.3252777778	2009-03-17 07:48:24	503101010	33.8911	25	33.8991	33.8991	0	33.8911	2	2	0	2	1	0	0	30.8309	30.8309	61.4979	0	PROCESSED	57545.8349652778	2016-06-06 20:02:21	55329	2010-05-13 00:00:00	54917.3115393518	2009-03-27 07:28:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031234	We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity.	GALACTIC DIFFUSE EMISSION	5	B	FARHAD YUSEF-ZADEH		USA	3	AO3	A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503101010/	Quick Look
154	K3/PSR J1420-6048	215.0274	-60.7627	214.105774	-60.533369	236.492647	-43.553641	313.55205119	0.26755801	90.771	54842.5598263889	2009-01-11 13:26:09	54843.8801388889	2009-01-12 21:07:24	503110010	50.269	50	50.269	50.269	0	50.269	1	1	0	1	1	0	0	50.0618	50.0618	114.0639	2	PROCESSED	57545.1792013889	2016-06-06 04:18:03	55328	2010-05-12 00:00:00	54854.3728703704	2009-01-23 08:56:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	033076	K3/PSR J1420-6048 is one of the TeV gamma-ray pulsar wind nebulae detected by HESS, which are thought to be main particle accelerators to the Galactic Cosmic rays. It was also detected by EGRET and its X-ray spectrum is very hard. In order to reveal the radiation mechanism, we propose to observe the extended source for 50 ksec on HXD nominal position and contamination source for 20 ksec on XIS nominal position. The main purpose of this observation is to obtain the hard X-ray spectrum up to about 40 keV.	GALACTIC DIFFUSE EMISSION	5	C	TETSUICHI KISHISHITA	ROGER ROMANI	JUS	3	AO3	SUZAKU OBSERVATION OF TEV GAMMA-RAY PWN K3/PSR J1420-6048	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503110010/	Quick Look
155	SGR_B2	266.8788	-28.4436	266.087557	-28.426518	267.23571	-5.032452	0.63679	-0.09938091	266.4718	55096.836412037	2009-09-22 20:04:26	55102.6667592593	2009-09-28 16:00:08	504004020	202.0945	200	202.0945	202.1025	0	202.0945	3	4	0	3	1	0	0	178.2831	178.2831	303.5437	4	PROCESSED	57548.82125	2016-06-09 19:42:36	55500	2010-10-31 00:00:00	55133.4505092593	2009-10-29 10:48:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040002	The Galactic center diffuse X-ray emission (GCDX) consists of the hot plasma, neutral iron line, and hard tail. While we have demonstrated the hot plasma truly extending, origins of the others are still under discussion. We found time variability of the neutral Fe line intensity and marginally detected neutral lines of S, Ar, and Ca from Sagittarius B2. Our purpose is to clearly detect the neutral lines of S, Ar, Ca, and time variability of the hard tail of the GCDX up to 40 keV. This observation will resolve the remaining mysteries of the GCDX.	GALACTIC DIFFUSE EMISSION	5	A	MASAYOSHI NOBUKAWA		JAP	4	AO4	SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION-	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504004020/	Quick Look
156	BLOWOUT1	312.2225	31.7347	311.709294	31.548551	327.170903	47.151978	74.53998499	-7.54540267	244.0864	55158.2754166667	2009-11-23 06:36:36	55158.9655555556	2009-11-23 23:10:24	504011010	24.1854	23	24.2014	24.1854	0	24.1934	2	2	0	2	1	0	0	19.4768	19.4768	59.6039	1	PROCESSED	57549.5243055556	2016-06-10 12:35:00	55545	2010-12-15 00:00:00	55176.2112731482	2009-12-11 05:04:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504011010/	Quick Look
157	BLOWOUT3	311.7021	31.3134	311.187829	31.12914	326.330215	46.937186	73.92913651	-7.4588166	242.4356	55160.1363888889	2009-11-25 03:16:24	55160.4723611111	2009-11-25 11:20:12	504013010	16.1599	16	16.1599	16.1599	0	16.1599	2	2	0	2	1	0	0	11.8101	11.8101	29.0219	0	PROCESSED	57549.5443634259	2016-06-10 13:03:53	55545	2010-12-15 00:00:00	55176.2365740741	2009-12-11 05:40:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504013010/	Quick Look
158	FESI1	313.4345	30.6099	312.913405	30.419428	327.914732	45.71047	74.31119672	-9.05841998	226.3696	55182.5546180556	2009-12-17 13:18:39	55183.3334837963	2009-12-18 08:00:13	504017010	32.2876	24	32.2876	32.2876	0	32.2876	2	2	0	2	1	0	0	27.2129	27.2129	67.2859	0	PROCESSED	57549.881099537	2016-06-10 21:08:47	55575	2011-01-14 00:00:00	55204.4679976852	2010-01-08 11:13:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504017010/	Quick Look
159	HESS J1731-347 N	262.8483	-34.6425	262.016963	-34.605825	263.993904	-11.350062	353.56257635	-0.49517094	91.6366	55244.8937037037	2010-02-17 21:26:56	55245.7189699074	2010-02-18 17:15:19	504032010	41.5263	40	41.5263	41.5263	0	41.5263	2	2	0	2	1	0	0	32.8653	32.8653	71.2719	0	PROCESSED	57550.6405555556	2016-06-11 15:22:24	55623	2011-03-03 00:00:00	55257.0108449074	2010-03-02 00:15:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040026	Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1731-347 is one of only 3 TeV SNRs which have a radio shell and possible thermal X-rays. With good statistics and low background observation of Suzaku XIS, we will detect thermal X-rays from the shell of HESS J1731-347 for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition.	GALACTIC DIFFUSE EMISSION	5	B	AYA BAMBA		JAP	4	AO4	DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504032010/	Quick Look
160	GALACTICDISC3-1	15.309	67.9759	14.492554	67.706941	51.801719	54.210388	123.85392042	5.12169353	244.2747	55214.8348148148	2010-01-18 20:02:08	55216.0225	2010-01-20 00:32:24	504038010	55.2279	50	55.2279	55.2279	0	55.2279	2	2	0	2	1	0	0	43.3329	43.3329	102.5998	2	PROCESSED	57550.2600231482	2016-06-11 06:14:26	55594	2011-02-02 00:00:00	55228.2005092593	2010-02-01 04:48:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040097	To elucidate the vertical structure of the yet-not-understood excess soft X-ray emission from the galactic disk, we propose to observe two offset directions from the plane along l = 123 degree. We expect the spectra contains the 0.75 keV emission component which we discovered in the energy spectra of two midplane observations. The proposed observations will strongly constrain the nature of the sources which are responsible for the excess emission, in particular the vertical distribution in the Galaxy.	GALACTIC DIFFUSE EMISSION	5	C	SHUNSUKE KIMURA		JAP	4	AO4	STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504038010/	Quick Look
161	ASO0505	339.5988	59.0734	339.120995	58.812928	20.160721	59.131044	106.55945745	0.49758229	62.7751	55001.185775463	2009-06-19 04:27:31	55001.7494675926	2009-06-19 17:59:14	504048010	26.3616	20	26.3696	26.3616	0	26.3776	2	2	0	2	1	0	0	23.8416	23.8416	48.6959	1	PROCESSED	57547.5983449074	2016-06-08 14:21:37	55381	2010-07-04 00:00:00	55015.2523148148	2009-07-03 06:03:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 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 DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504048010/	Quick Look
162	ASO0418	279.775	-5.7085	279.106672	-5.754175	280.186655	17.387028	26.44714681	0.13153934	86.843	54934.6472800926	2009-04-13 15:32:05	54935.7578587963	2009-04-14 18:11:19	504052010	41.0684	40	41.0802	41.0844	0	41.0684	2	2	0	2	1	0	0	33.5258	33.5258	95.9378	0	PROCESSED	57546.1671296296	2016-06-07 04:00:40	55324	2010-05-08 00:00:00	54949.5662268518	2009-04-28 13:35:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040112	We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504052010/	Quick Look
163	ASO0215	154.6836	-58.9426	154.241353	-58.691332	196.521873	-60.887637	284.32918046	-1.70077172	314.5017	55019.3141782407	2009-07-07 07:32:25	55020.3404976852	2009-07-08 08:10:19	504053010	40.0868	40	40.0868	40.0868	0	40.0868	2	2	0	2	1	0	0	35.4782	35.4782	88.6598	0	PROCESSED	57547.8126851852	2016-06-08 19:30:16	55399	2010-07-22 00:00:00	55029.2468055556	2009-07-17 05:55:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040112	We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504053010/	Quick Look
164	ASO0319	224.8822	-60.8823	223.89321	-60.683278	242.498215	-41.674426	317.89227503	-1.78687667	277.7774	55049.7078125	2009-08-06 16:59:15	55051.0238425926	2009-08-08 00:34:20	504055010	42.3613	40	42.3613	42.3668	0	42.3773	2	2	0	2	1	0	0	37.5233	37.5233	113.6859	0	PROCESSED	57548.1027083333	2016-06-09 02:27:54	55430	2010-08-22 00:00:00	55062.2941782407	2009-08-19 07:03:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040112	We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504055010/	Quick Look
165	NEP #2	270.0521	66.5655	270.053494	66.565223	19.553337	89.984047	96.38949161	29.79071779	194.6438	55172.5015162037	2009-12-07 12:02:11	55173.6411342593	2009-12-08 15:23:14	504072010	48.6977	50	48.6977	48.6977	0	48.6977	2	2	0	2	1	0	0	38.4582	38.4582	98.456	1	PROCESSED	57549.730775463	2016-06-10 17:32:19	54922	2009-04-01 00:00:00	55190.01875	2009-12-25 00:27:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041101	We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe.	GALACTIC DIFFUSE EMISSION	5	A	STEVEN SNOWDEN		USA	4	AO4	OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504072010/	Quick Look
166	HESS J1809-193A	273.0012	-19.0034	272.264617	-19.016192	272.836277	4.407781	11.60922783	-0.25253702	270.0939	55083.2051967593	2009-09-09 04:55:29	55084.4828009259	2009-09-10 11:35:14	504077010	52.1109	50	52.1745	52.1908	0	52.1109	3	3	0	3	1	0	0	44.109	44.109	110.376	1	PROCESSED	57548.5474189815	2016-06-09 13:08:17	55475	2010-10-06 00:00:00	55109.4207638889	2009-10-05 10:05:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041303	We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background.	GALACTIC DIFFUSE EMISSION	5	A	OLEG KARGALTSEV		USA	4	AO4	CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504077010/	Quick Look
167	G156.2+5.7 (S)	74.9073	51.0204	73.935792	50.94566	79.297666	28.139899	156.85145441	5.28162006	265.6871	55259.9832407407	2010-03-04 23:35:52	55261.1495833333	2010-03-06 03:35:24	504080010	52.6413	50	52.6493	52.6413	0	52.6493	2	2	0	2	1	0	0	47.6566	47.6566	100.7578	0	PROCESSED	57550.7899189815	2016-06-11 18:57:29	55689	2011-05-08 00:00:00	55323.2891666667	2010-05-07 06:56:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041311	The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks.	GALACTIC DIFFUSE EMISSION	5	C	SATORU KATSUDA		USA	4	AO4	REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504080010/	Quick Look
168	330.2+1.0	240.2338	-51.5878	239.290441	-51.447552	249.060918	-30.286354	330.14022152	0.98429318	285.0004	55081.4851273148	2009-09-07 11:38:35	55082.1453472222	2009-09-08 03:29:18	504083020	30.8896	30	30.8896	30.8896	0	30.8971	2	2	0	2	1	0	0	27.0764	27.0764	57.0379	0	PROCESSED	57548.4451736111	2016-06-09 10:41:03	55458	2010-09-19 00:00:00	55092.1620949074	2009-09-18 03:53:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041312	Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity.	GALACTIC DIFFUSE EMISSION	5	B	GLENN ALLEN		USA	4	AO4	MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504083020/	Quick Look
169	NGC 6888	302.9954	38.2382	302.538596	38.087534	320.045193	56.092572	75.36419968	2.38310331	253.873	55139.4126388889	2009-11-04 09:54:12	55141.3127777778	2009-11-06 07:30:24	504085010	77.349	75	77.461	77.349	0	77.461	3	2	0	2	1	0	0	62.1002	62.1002	164.1558	0	PROCESSED	57549.1334837963	2016-06-10 03:12:13	55518	2010-11-18 00:00:00	55152.1455671296	2009-11-17 03:29:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041321	Fast winds from massive stars create large cavities in the surrounding interstellar medium filled with hot gas, known as Wind-Blown Bubbles (WBB). We propose to obtain XIS imaging spectroscopy of the prototype WBB NGC 6888. Thanks to the XIS excellent sensitivity and energy resolution in the soft X-ray band, we will: (i) obtain a high quality CCD spectrum which can be used to constrain the temperature of the hot plasma and the efficiency of thermal conduction across the bubble wall, (ii) determine the spatial distribution and properties of X-ray emitting plasma, (iii) therefore, test and refine shock physics models of bubbles by a direct confrontation of their results with observations.	GALACTIC DIFFUSE EMISSION	5	A	SVETOZAR ZHEKOV		USA	4	AO4	X-RAYS FROM THE PROTOTYPE WIND-BLOWN BUBBLE NGC 6888	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504085010/	Quick Look
170	MRK 421 OFFSET	166.8026	37.7335	166.111285	38.004105	152.017379	29.315723	180.50489089	65.69633084	129.0398	55144.0655092593	2009-11-09 01:34:20	55145.8091087963	2009-11-10 19:25:07	504086010	75.2595	75	75.2675	75.2595	0	75.2675	2	2	0	2	1	0	0	51.94	51.94	150.6288	2	PROCESSED	57549.2648148148	2016-06-10 06:21:20	55542	2010-12-12 00:00:00	55176.2291319444	2009-12-11 05:29:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041324	The OVII, OVIII, and NeIX absorption lines at z~0 have been discovered in the Chandra/XMM spectra of several bright AGNs, but the location of these absorptions has been debated since their discoveries. Here we request Suzaku observations of the soft X-ray background emission in the vicinity of Mrk 421, to conduct a joint analysis of the emission data with the extensive Chandra absorption data. This analysis will naturally yield an effective length of the absorbing/emitting gas. We have performed pilot studies and obtained a scale length of several kpc for the hot absorbing/emitting gas toward LMC X-3 and Mrk 421. The requested Suzaku observations are particular important to check these results and to further test the models we have developed in our study.	GALACTIC DIFFUSE EMISSION	5	B	YANGSEN YAO		USA	4	AO4	A JOINT X-RAY ABSORPTION AND EMISSION STUDY OF THE HOT GAS TOWARD MRK 421	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504086010/	Quick Look
171	KEPLER_BG_GE	263.5357	-20.2632	262.792974	-20.230061	263.919291	3.041451	5.99779838	6.79710869	273.0028	55072.0030208333	2009-08-29 00:04:21	55072.5002662037	2009-08-29 12:00:23	504101020	24.7227	60	24.7467	24.7387	0	24.7227	2	2	0	2	1	0	0	19.2528	19.2528	42.9559	0	PROCESSED	57548.3891550926	2016-06-09 09:20:23	54922	2009-04-01 00:00:00	55109.4155324074	2009-10-05 09:58:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	4	AO4	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504101020/	Quick Look
172	KEPLER_BG_GW	261.806	-22.7684	261.049806	-22.726898	262.438757	0.457902	2.99933771	6.7960859	273.0885	55109.2984143518	2009-10-05 07:09:43	55111.1057175926	2009-10-07 02:32:14	504102010	65.2949	60	65.3029	65.2949	0	65.3029	2	2	0	2	1	0	0	50.7821	50.7821	156.128	1	PROCESSED	57548.8038425926	2016-06-09 19:17:32	54922	2009-04-01 00:00:00	55125.6963888889	2009-10-21 16:42:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	4	AO4	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504102010/	Quick Look
173	KEPLER_BG_GS	263.1005	-22.949	262.342899	-22.913725	263.639389	0.339875	3.49961978	5.69692486	272.6396	55107.43	2009-10-03 10:19:12	55109.2973842593	2009-10-05 07:08:14	504104010	67.2508	60	67.2508	67.2805	0	67.2748	2	2	0	2	1	0	0	53.1585	53.1585	161.3298	1	PROCESSED	57548.7538425926	2016-06-09 18:05:32	54922	2009-04-01 00:00:00	55125.3521180556	2009-10-21 08:27:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	4	AO4	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504104010/	Quick Look
174	3C_391	282.3812	-0.9417	281.735823	-0.99987	283.351934	21.926784	31.87573789	-0.00377867	261.9952	55491.0759722222	2010-10-22 01:49:24	55493.8224537037	2010-10-24 19:44:20	505007010	99.3887	100	99.4607	99.3887	0	99.4687	2	2	0	2	1	0	0	89.374	89.374	237.2779	2	PROCESSED	57553.8698032407	2016-06-14 20:52:31	55287	2010-04-01 00:00:00	55502.3356597222	2010-11-02 08:03:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050002	We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505007010/	Quick Look
175	CYGNUS LOOP 1	313.2462	32.1399	312.732912	31.950084	328.580357	47.179033	75.40840203	-7.96786776	81.7816	55300.7096759259	2010-04-14 17:01:56	55301.0293402778	2010-04-15 00:42:15	505009010	15.9992	13	15.9992	15.9992	0	15.9992	2	2	0	2	1	0	0	12.242	12.242	27.612	0	PROCESSED	57551.2105787037	2016-06-12 05:03:14	55287	2010-04-01 00:00:00	55362.3098726852	2010-06-15 07:26:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505009010/	Quick Look
176	CYGNUS LOOP 2	312.7259	32.1633	312.213805	31.975338	327.998937	47.37656	75.14683323	-7.61088939	81.0273	55301.0300925926	2010-04-15 00:43:20	55301.2897569444	2010-04-15 06:57:15	505010010	12.932	10	12.932	12.932	0	12.932	1	1	0	1	1	0	0	11.924	11.924	22.4319	0	PROCESSED	57551.2143402778	2016-06-12 05:08:39	55287	2010-04-01 00:00:00	55362.2959375	2010-06-15 07:06:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505010010/	Quick Look
177	CYGNUS LOOP 3	312.9529	31.9301	312.439181	31.741329	328.122092	47.08601	75.08571271	-7.90709143	81.0389	55301.2902777778	2010-04-15 06:58:00	55301.6209953704	2010-04-15 14:54:14	505011010	13.4448	12	13.4448	13.4448	0	13.4448	2	2	0	2	1	0	0	10.427	10.427	28.5719	0	PROCESSED	57551.2233333333	2016-06-12 05:21:36	55287	2010-04-01 00:00:00	55362.3557060185	2010-06-15 08:32:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505011010/	Quick Look
178	CYGNUS LOOP 10	314.1171	30.7461	313.595298	30.553225	328.763604	45.604555	74.79486269	-9.42625359	82.0017	55328.2812152778	2010-05-12 06:44:57	55328.6981134259	2010-05-12 16:45:17	505018010	16.268	16	16.276	16.276	0	16.268	2	2	0	2	1	0	0	12.6551	12.6551	36.012	0	PROCESSED	57551.4785069444	2016-06-12 11:29:03	55287	2010-04-01 00:00:00	55393.3335069445	2010-07-16 08:00:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505018010/	Quick Look
179	G22.0+0.0	277.823	-9.7151	277.134886	-9.751345	277.921132	13.510599	22.00005623	0.00370699	89.3658	55302.6023842593	2010-04-16 14:27:26	55303.7272222222	2010-04-17 17:27:12	505025010	50.5294	50	50.5294	50.5294	0	50.5294	2	2	0	2	1	0	0	44.6208	44.6208	97.1598	0	PROCESSED	57551.270775463	2016-06-12 06:29:55	55737	2011-06-25 00:00:00	55375.7533101852	2010-06-28 18:04:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050009	ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature.	GALACTIC DIFFUSE EMISSION	5	B	SHIGEO YAMAUCHI		JAP	5	AO5	SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505025010/	Quick Look
180	G37.0-0.1	284.8009	3.5813	284.176842	3.511637	286.494967	26.178305	37.00394757	-0.09218404	68.6266	55303.7327893518	2010-04-17 17:35:13	55304.8814583333	2010-04-18 21:09:18	505027010	50.9694	50	50.9774	50.9774	0	50.9694	2	2	0	2	1	0	0	45.3361	45.3361	99.23	1	PROCESSED	57551.2689699074	2016-06-12 06:27:19	55693	2011-05-12 00:00:00	55326.2903125	2010-05-10 06:58:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050009	ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature.	GALACTIC DIFFUSE EMISSION	5	B	SHIGEO YAMAUCHI		JAP	5	AO5	SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505027010/	Quick Look
181	SGR_C	266.2461	-29.3903	265.44899	-29.370135	266.702279	-5.992122	359.54016882	-0.1184914	267.0744	55464.5256481482	2010-09-25 12:36:56	55466.608599537	2010-09-27 14:36:23	505031010	99.916	100	99.9561	99.916	0	99.956	3	2	0	2	1	0	0	89.0712	89.0712	179.9499	2	PROCESSED	57553.5757175926	2016-06-14 13:49:02	55853	2011-10-19 00:00:00	55484.3402777778	2010-10-15 08:10:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050018	The Sagittarius C Complex (Sgr C) @is composed of many giant molecular clouds (MCs) in two distinct velocity zones, indicating two separate line-of-sight positions of the MCs. Past X-ray flares of Sgr A* likely produced the FeI 6.4 keV emission in the MCs (XRN: X-ray Reflection Nebulae). In Sgr C, the XRN have been solely found in one of the velocity zones. We hence propose to find new XRN in the other velocity zone, which is possibly located at the different distance from the known XRN. With the Suzaku observation, we will determine the 3-dimensional positions of the XRN. Since the presence (or absence) of the XRN largely depends on the epoch of the Sgr A* flares and the 3-dimensional positions of the MCs, Sgr C is a "Rosetta Stone" of the origin and production of the XRN.	GALACTIC DIFFUSE EMISSION	5	A	MASAYOSHI NOBUKAWA		JAP	5	AO5	THE SAGITTARIUS C COMPLEX A ROSETTA STONE OF THE PAST ACTIVITY OF SAGITTARIUS A*	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505031010/	Quick Look
182	BLOWOUT SHELL 1	311.9978	28.9736	311.471635	28.788286	325.391021	44.676168	72.22846422	-9.10440661	48.7676	55360.0953587963	2010-06-13 02:17:19	55361.2627546296	2010-06-14 06:18:22	505055010	52.1945	50	52.2185	52.1945	0	52.2185	1	1	0	1	1	0	0	43.6927	43.6927	100.8559	1	PROCESSED	57552.0261226852	2016-06-13 00:37:37	55741	2011-06-29 00:00:00	55375.7594907407	2010-06-28 18:13:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050088	The Cygnus Loop is a typical shell-like middle-aged SNR. The origin of this SNR is considered to be a cavity explosion. Many previous studies show the abundance of the Cygnus Loop's shell is wholly low (0.2 solar) while that of the ambient medium is typically 0.5 solar. Based on our previous observations, we found some shell regions show 0.5 solar abundances which are consistent with that of the ISM. To explain this result, we formed a hypothesis that the cavity wall density is low in such region and that the forward shock is now propagating outside the cavity, interacting with the ambient medium. In order to verify this hypothesis, we propose to observe the shell of the blowout region which originates from a large break of the cavity wall. We propose to observe two regions for 100ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROYUKI UCHIDA		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP BLOWOUT REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505055010/	Quick Look
183	BLOWOUT SHELL 2	312.2035	28.7297	311.67582	28.543644	325.497444	44.382569	72.14669544	-9.39669734	48.0881	55361.263599537	2010-06-14 06:19:35	55362.5155439815	2010-06-15 12:22:23	505056010	52.0698	50	52.0698	52.0698	0	52.0698	2	2	0	2	1	0	0	46.0827	46.0827	108.1558	1	PROCESSED	57552.3493634259	2016-06-13 08:23:05	55741	2011-06-29 00:00:00	55375.7627893518	2010-06-28 18:18:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050088	The Cygnus Loop is a typical shell-like middle-aged SNR. The origin of this SNR is considered to be a cavity explosion. Many previous studies show the abundance of the Cygnus Loop's shell is wholly low (0.2 solar) while that of the ambient medium is typically 0.5 solar. Based on our previous observations, we found some shell regions show 0.5 solar abundances which are consistent with that of the ISM. To explain this result, we formed a hypothesis that the cavity wall density is low in such region and that the forward shock is now propagating outside the cavity, interacting with the ambient medium. In order to verify this hypothesis, we propose to observe the shell of the blowout region which originates from a large break of the cavity wall. We propose to observe two regions for 100ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROYUKI UCHIDA		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP BLOWOUT REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505056010/	Quick Look
184	HE FOCUSING CONE	49.5928	10.9507	48.911727	10.768982	50.111751	-7.072007	170.97872575	-37.85410489	253.7002	55591.1307291667	2011-01-30 03:08:15	55593.7710763889	2011-02-01 18:30:21	505062010	100.1678	100	100.1678	100.1678	0	100.1678	2	2	0	2	1	0	0	82.7852	82.7852	228.1037	2	PROCESSED	57600.8639351852	2016-07-31 20:44:04	55973	2012-02-16 00:00:00	55607.305462963	2011-02-15 07:19:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050129	We propose the observation though the Helium Focusng Cone. This region seems to make the strong enhancement of Solarwind Charge exchange and cause the annual variation of it. We develop the best observation of the cone by using the area where the abosorption by molecular cloud is huge. By this observation, we investigate the mistery of the emission of Our Galaxy.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI YOSHITAKE		JAP	5	AO5	OBSERVATION THROUGH THE HELIUM FOCUSING CONE: SEARCH FOR THE VARIABILITY OF THE HELIOSPHERIC SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505062010/	Quick Look
185	0548-70.4	86.9619	-70.4173	87.103378	-70.431737	284.612052	-85.985846	280.90214015	-30.75163284	12.6051	55378.8779861111	2010-07-01 21:04:18	55381.6286689815	2010-07-04 15:05:17	505065010	103.6746	100	103.6746	103.6746	0	103.6746	2	2	0	2	1	0	0	156.9716	156.9716	237.6358	1	PROCESSED	57552.5583912037	2016-06-13 13:24:05	55287	2010-04-01 00:00:00	55434.3854513889	2010-08-26 09:15:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051102	Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors.	GALACTIC DIFFUSE EMISSION	5	B	KAZIMIERZ BORKOWSKI		USA	5	AO5	TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505065010/	Quick Look
186	VELA SNR CB2	130.2058	-44.7742	129.776213	-44.595251	154.639113	-59.522265	263.81853128	-1.77251278	293.5729	55318.5746412037	2010-05-02 13:47:29	55318.9238425926	2010-05-02 22:10:20	505069010	19.3805	20	19.4125	19.4045	0	19.3805	1	1	0	1	1	0	0	18.8298	18.8298	30.1679	0	PROCESSED	57551.3535763889	2016-06-12 08:29:09	55696	2011-05-15 00:00:00	55330.2121643518	2010-05-14 05:05:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051304	The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	5	AO5	IRON-RICH EJECTA BULLET IN THE VELA SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505069010/	Quick Look
187	AX J1714.1-3912	258.5249	-39.1972	257.66219	-39.139743	260.755226	-16.122974	347.85266774	-0.22742448	85.6964	55608.0538078704	2011-02-16 01:17:29	55608.9654050926	2011-02-16 23:10:11	505076010	32.6017	30	32.6017	32.6017	0	32.6017	2	2	0	2	1	0	0	28.3362	28.3362	78.7579	1	PROCESSED	57600.9625115741	2016-07-31 23:06:01	55988	2012-03-02 00:00:00	55621.1409027778	2011-03-01 03:22:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052012	Molecular clouds are predicted to emit strong non-thermal X-rays when they are close to particle-accelerating SNRs, but this emission has not been confirmed yet. We propose to observe the non-thermal X-ray source AX J1714.1-3912 to investigate its relationship with the SNR RX J1713.7-3946. ASCA observations have shown that the hard spectrum of the source may be associated with bremsstrahlung emission from particles accelerated in the SNR and diffusing in a nearby molecular cloud. This emission has never been observed in other SNRs. However, the association of the source with the remnant is still controversial and the ASCA data do not allow us to constrain the spectral properties. We aim at verifying the association with the remnant and at investigating the physical origin of the emission.	GALACTIC DIFFUSE EMISSION	5	A	MARCO MICELI		EUR	5	AO5	INVESTIGATING THE PHYSICAL ORIGIN OF AX J1714.1-3912	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505076010/	Quick Look
188	GALACTIC_BULGE3	267.9488	-29.7963	267.148788	-29.784389	268.199437	-6.368042	359.95634845	-1.5962466	107.1729	55624.8013310185	2011-03-04 19:13:55	55626.2292939815	2011-03-06 05:30:11	505078010	51.2756	50	51.2756	51.2756	0	51.2756	2	2	0	2	1	0	0	39.3124	39.3124	123.3618	0	PROCESSED	57601.0957407407	2016-08-01 02:17:52	55287	2010-04-01 00:00:00	55642.1205787037	2011-03-22 02:53:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505078010/	Quick Look
189	GALACTIC_BULGE15	265.6963	-32.7784	264.876935	-32.755516	266.323781	-9.39206	356.40742505	-1.49294303	89.8786	55626.2338425926	2011-03-06 05:36:44	55627.5424884259	2011-03-07 13:01:11	505084010	50.3097	50	50.3172	50.3097	0	50.3252	1	1	0	1	1	0	0	37.5095	37.5095	113.0559	0	PROCESSED	57601.1030439815	2016-08-01 02:28:23	55287	2010-04-01 00:00:00	55645.2697222222	2011-03-25 06:28:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505084010/	Quick Look
190	GALACTIC_BULGE16	266.5113	-33.2224	265.68867	-33.203457	267.02907	-9.817155	356.38592507	-2.30771737	275.4625	55482.2533217593	2010-10-13 06:04:47	55483.5626967593	2010-10-14 13:30:17	505085010	55.0315	50	55.0315	55.0315	0	55.0315	2	2	0	2	1	0	0	48.6341	48.6341	113.1139	1	PROCESSED	57553.750787037	2016-06-14 18:01:08	55287	2010-04-01 00:00:00	55502.290150463	2010-11-02 06:57:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505085010/	Quick Look
191	GALACTIC_BULGE17	267.7467	-33.8391	266.919516	-33.82614	268.087567	-10.412886	356.3863118	-3.50805248	275.261	55483.5637731482	2010-10-14 13:31:50	55485.0627893518	2010-10-16 01:30:25	505086010	53.1266	50	53.1266	54.0895	0	54.0895	2	2	0	2	1	0	0	46.2769	46.2769	129.4938	1	PROCESSED	57553.7652430556	2016-06-14 18:21:57	55287	2010-04-01 00:00:00	55508.2025694444	2010-11-08 04:51:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505086010/	Quick Look
192	HESS J1841-55 3	280.1471	-5.609	279.479279	-5.656459	280.581257	17.459575	26.70525302	-0.15199861	87.0298	55647.6397685185	2011-03-27 15:21:16	55648.791875	2011-03-28 19:00:18	505090010	49.549	50	49.581	49.549	0	49.581	2	2	0	2	1	0	0	42.7935	42.7935	99.5239	1	PROCESSED	57601.3633101852	2016-08-01 08:43:10	55287	2010-04-01 00:00:00	55666.2655439815	2011-04-15 06:22:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505090010/	Quick Look
193	BD+43 3654	308.4185	44.0658	307.988834	43.893641	331.745866	59.550103	82.48241574	2.36274642	104.8287	55655.0785416667	2011-04-04 01:53:06	55657.0925231482	2011-04-06 02:13:14	506004010	97.0478	100	98.9638	97.0478	0	98.9638	3	2	0	2	1	0	0	88.9256	88.9256	173.9877	0	PROCESSED	57601.4465972222	2016-08-01 10:43:06	56037	2012-04-20 00:00:00	55670.3073842593	2011-04-19 07:22:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060010	It is very important to search for possible particle-acceleration sites among the astrophysical objects. Very recently, synchrotron emission has been discovered with the VLA radio observation from a bow shock region of a runaway star, BD+43 3654, having a very fast stellar wind whose velocity reaches up to 2300 km/s. The maximum energy is estimated to be about 10 TeV, and thus the emission should come to the X-ray band. Here, we propose to perform the 100 ksec observation of BD+43 3654 with Suzaku, in order to determine the strength of the shock from the temperature of the post-shock plasma and to determine the maximum energy of the accelerated electrons.	GALACTIC DIFFUSE EMISSION	5	A	YUKIKATSU TERADA		JAP	6	AO6	SUZAKU OBSERVATION OF NON-THERMAL EMISSION FROM A BOW SHOCK REGION OF A RUNAWAY STAR, BD+43 3654	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506004010/	Quick Look
194	JUPITER	28.9811	10.6021	28.315769	10.357786	30.678261	-1.183373	147.5984875	-49.15640747	249.1843	55937.2038773148	2012-01-11 04:53:35	55938.208599537	2012-01-12 05:00:23	506006030	34.8942	160	34.9022	34.9102	0	34.8942	2	2	0	2	1	0	0	32.2081	32.2081	86.7918	2	PROCESSED	57604.3101273148	2016-08-04 07:26:35	56319	2013-01-27 00:00:00	55952.170787037	2012-01-26 04:05:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060017	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter.	GALACTIC DIFFUSE EMISSION	5	B	KUMI ISHIKAWA		JAP	6	AO6	STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006030/	Quick Look
195	CYGNUS LOOP W-B-S	311.1967	30.3719	310.678738	30.189494	325.222144	46.233696	72.9110541	-7.69596159	71.021	55693.7715277778	2011-05-12 18:31:00	55694.9794212963	2011-05-13 23:30:22	506008010	55.6499	56	55.6499	55.6499	0	55.6499	2	2	0	2	1	0	0	49.8516	49.8516	104.3259	1	PROCESSED	57602.0472916667	2016-08-02 01:08:06	56072	2012-05-25 00:00:00	55705.1847800926	2011-05-24 04:26:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060042	The Cygnus Loop is a prototypical middle-aged SNR. Based on our previous observations, the shell region shows relatively low temperature with low metal abundance. The interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Its abundance non-uniformity indicates the asymmetric explosion. There are two blow-out features: a south-break with one degree diameter and a west-break with half degree diameter. The west-break shows a half-moon shape indicating a rapid expansion in a tenuous plasma. We propose to observe the west-break with SUZAKU for 100 ksec. The plasma in the west-break must be a pure fossil plasma of the SN. We want to study the plasma structure that is almost free from obscuration by the ISM.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	6	AO6	HUNT FOR THE FOSSIL OF THE PROGENITOR STAR IN THE WEST BREAK OF THE CYGNUS LOOP SUPERNOVA REMNANT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506008010/	Quick Look
196	HESSJ1857-B	284.5485	2.7494	283.920534	2.680934	286.113501	25.379812	36.14879968	-0.24805898	252.48	55866.7917592593	2011-11-01 19:00:08	55867.6946990741	2011-11-02 16:40:22	506020010	40.6869	40	40.6869	40.6949	0	40.6949	2	2	0	2	1	0	0	40.0513	40.0513	78.0119	0	PROCESSED	57603.6841435185	2016-08-03 16:25:10	56246	2012-11-15 00:00:00	55879.1725	2011-11-14 04:08:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060061	Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	6	AO6	ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506020010/	Quick Look
197	NGC 7618	349.8326	42.9144	349.23867	42.640678	11.92237	42.546584	105.51742003	-16.82119292	269.9991	55911.4056828704	2011-12-16 09:44:11	55913.6161458333	2011-12-18 14:47:15	506027010	101.1772	100	101.1852	101.1772	0	101.1852	2	2	0	2	1	0	0	95.774	95.774	190.9399	0	PROCESSED	57604.196712963	2016-08-04 04:43:16	56289	2012-12-28 00:00:00	55922.1112847222	2011-12-27 02:40:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060073	We propose to observe nearby merging galaxy group NGC 7618. The asymmetric X-ray shape with a tail and a sharp brightness discontinuity were discoverd by observations of ASCA and Chandra. This is due to a merging with an another galaxy group, UGC 12491, which has similar mass of NGC 7618. The pair is in the primary stage of merging, then we need to obtain the information of the gas outside region to clarify the process of the merging. By taking advantage of low background and high energy resolution of XIS, we estimate accurately distribuion of temperature and metal abundances around both galaxy groups. Then we aim to clarify the process of the merging system of the galaxy groups.	GALACTIC DIFFUSE EMISSION	5	C	KATSUHIRO HAYASHI		JAP	6	AO6	OBSERVATION OF NEARBY MERGING GALAXY GROUP NGC 7618	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506027010/	Quick Look
198	VELA PWN E5	130.8405	-45.4455	130.413883	-45.264192	156.083116	-59.869195	264.62375514	-1.83200273	304.5067	55712.7368402778	2011-05-31 17:41:03	55712.9570601852	2011-05-31 22:58:10	506048010	15.9196	15	15.9196	15.9196	0	15.9436	1	1	0	1	1	0	0	11.9129	11.9129	19.0159	0	PROCESSED	57602.1724305556	2016-08-02 04:08:18	56093	2012-06-15 00:00:00	55726.0610185185	2011-06-14 01:27:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506048010/	Quick Look
199	VELA PWN E7	131.6969	-45.5129	131.268004	-45.328458	157.17001	-59.613979	265.05012769	-1.40367097	303.5042	55713.2300925926	2011-06-01 05:31:20	55713.4688310185	2011-06-01 11:15:07	506050010	13.0454	15	13.0494	13.0454	0	13.0534	1	1	0	1	1	0	0	11.0751	11.0751	20.622	0	PROCESSED	57602.181875	2016-08-02 04:21:54	56093	2012-06-15 00:00:00	55726.0999768518	2011-06-14 02:23:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506050010/	Quick Look
200	G236+38 OFF	149.4117	1.4719	148.767122	1.710754	151.004118	-10.298746	237.07053965	41.11953464	293.1755	55719.6375462963	2011-06-07 15:18:04	55721.2780092593	2011-06-09 06:40:20	506056010	70.8135	70	70.8215	70.8295	0	70.8135	2	2	0	2	1	0	0	64.4444	64.4444	141.7278	0	PROCESSED	57602.2364583333	2016-08-02 05:40:30	56127	2012-07-19 00:00:00	55757.6968518518	2011-07-15 16:43:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061321	Interstellar clouds cast shadows in the soft X-ray background (SXRB). Observations of these shadows enable us to disentangle the various components of the SXRB. Unfortunately, to date, shadowing observations with XMM or Suzaku have only been published for three directions, all in the southern Galactic hemisphere. We propose two new pairs of on- and off-cloud shadowing observations, in order to sample the northern Galactic hemisphere. Our particular goal is to obtain accurate X-ray spectra of the Galactic halo, which we will compare with the predictions of models of galactic fountains and infalling extragalactic material.	GALACTIC DIFFUSE EMISSION	5	B	DAVID HENLEY		USA	6	AO6	UNDERSTANDING THE ORIGIN OF THE GALACTIC HALO USING SHADOWING OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506056010/	Quick Look
201	KES 27	237.1872	-53.7777	236.229597	-53.624833	247.581589	-32.858337	327.32071311	0.47884394	101.6269	55983.5400231482	2012-02-26 12:57:38	55985.4633217593	2012-02-28 11:07:11	506063010	109.3535	120	109.4015	109.3535	0	109.4015	3	2	0	2	1	0	0	115.3321	115.3321	166.148	4	PROCESSED	57604.7717592593	2016-08-04 18:31:20	55652	2011-04-01 00:00:00	55995.1904976852	2012-03-09 04:34:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506063010/	Quick Look
202	G349.7+0.2	259.4954	-37.4452	258.645482	-37.392398	261.399155	-14.316641	349.72102569	0.17051597	282.4112	55833.4324537037	2011-09-29 10:22:44	55838.1341898148	2011-10-04 03:13:14	506064010	160.4024	160	160.4264	160.4024	0	160.4344	2	2	0	2	1	0	0	144.6151	144.6151	404.22	5	PROCESSED	57603.3931134259	2016-08-03 09:26:05	55652	2011-04-01 00:00:00	55858.5356018518	2011-10-24 12:51:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506064010/	Quick Look
203	FERMI_BUBBLE_N2	234.4045	4.1242	233.780349	4.287466	230.936286	22.866796	10.25580888	44.20015183	287.5	56145.3990740741	2012-08-06 09:34:40	56145.971099537	2012-08-06 23:18:23	507002010	22.491	20	22.491	22.491	0	22.491	2	2	0	2	1	0	0	22.5	22.5	49.4059	0	PROCESSED	57606.7805555556	2016-08-06 18:44:00	56630	2013-12-04 00:00:00	56264.5602662037	2012-12-03 13:26:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507002010/	Quick Look
204	FERMI_BUBBLE_N3	234.0339	6.0902	233.417441	6.254904	230.000126	24.67426	12.27048516	45.60209416	287.4996	56145.9724537037	2012-08-06 23:20:20	56146.4377893518	2012-08-07 10:30:25	507003010	22.4846	20	22.4846	22.5086	0	22.4926	2	2	0	2	1	0	0	19.836	19.836	40.1959	0	PROCESSED	57606.7866782407	2016-08-06 18:52:49	56535	2013-08-31 00:00:00	56169.009837963	2012-08-30 00:14:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507003010/	Quick Look
205	FERMI_BUBBLE_N6	233.4001	9.0706	232.795243	9.23775	228.456067	27.38567	15.47217439	47.71191257	287.5008	56147.4330324074	2012-08-08 10:23:34	56147.9606134259	2012-08-08 23:03:17	507006010	20.607	20	20.607	20.6246	0	20.619	2	2	0	2	1	0	0	20.3045	20.3045	45.58	0	PROCESSED	57606.8039467593	2016-08-06 19:17:41	56626	2013-11-30 00:00:00	56260.4951851852	2012-11-29 11:53:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507006010/	Quick Look
206	FERMI_BUBBLE_S6	326.677	-46.8481	325.870677	-47.079705	311.980005	-31.325121	351.64382858	-48.94656928	44.0056	56037.1166087963	2012-04-20 02:47:55	56037.6009027778	2012-04-20 14:25:18	507014010	19.6439	20	19.6519	19.6439	0	19.6599	1	1	0	1	1	0	0	14.1827	14.1827	41.8399	1	PROCESSED	57605.2222916667	2016-08-05 05:20:06	56420	2013-05-08 00:00:00	56054.1845833333	2012-05-07 04:25:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507014010/	Quick Look
207	GC_SOUTH_2	268.3751	-29.7084	267.575601	-29.69856	268.570633	-6.275404	0.22024801	-1.8703349	273.7998	56192.7899421296	2012-09-22 18:57:31	56194.081412037	2012-09-24 01:57:14	507029010	52.4469	50	52.4629	52.4469	0	52.4549	1	1	0	1	1	0	0	45.2307	45.2307	111.5759	1	PROCESSED	57607.1634259259	2016-08-07 03:55:20	56689	2014-02-01 00:00:00	56321.5121875	2013-01-29 12:17:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070042	We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation.	GALACTIC DIFFUSE EMISSION	5	A	SHINYA NAKASHIMA		JAP	7	AO7	OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507029010/	Quick Look
208	G298.6-0.0	183.3873	-62.6234	182.718198	-62.34531	219.474963	-53.500968	298.59191859	-0.0713547	133.8706	56341.7597222222	2013-02-18 18:14:00	56342.6981712963	2013-02-19 16:45:22	507037020	39.7247	35	39.7247	39.7247	0	39.7247	3	2	0	2	1	0	0	36.2621	36.2621	81.0699	0	PROCESSED	57610.644849537	2016-08-10 15:28:35	56721	2014-03-05 00:00:00	56362.8029861111	2013-03-11 19:16:18	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070047	A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem.	GALACTIC DIFFUSE EMISSION	5	B	AYA BAMBA		JAP	7	AO7	SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507037020/	Quick Look
209	MSH15-56_SW	238.0528	-56.3239	237.060386	-56.174494	248.949341	-35.191477	326.11105465	-1.81589779	86.2015	56326.3325	2013-02-03 07:58:48	56327.8577314815	2013-02-04 20:35:08	507039010	86.0122	100	86.0122	86.0122	0	86.0122	2	2	0	2	1	0	0	88.3912	88.3912	131.7719	2	PROCESSED	57610.534849537	2016-08-10 12:50:11	56714	2014-02-26 00:00:00	56345.5312847222	2013-02-22 12:45:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070055	The magnetic field upstream the shock front of the SN blast wave is the key parameter for discussing particle acceleration. In this study we try to constrain the upstream magnetic field and its amplification based on the ionization parameter of heated ISM just behind the shock. For this purpose, we propose a 100 ks XIS observation of an middle aged SNR MSH 15-56 with non-thermal filaments and an anomalously large ionization age for its dynamical age.	GALACTIC DIFFUSE EMISSION	5	C	YOICHI YATSU		JAP	7	AO7	A STUDY OF PARTICLE ACCELERATION BASED ON THE THERMAL PLASMA BEHIND THE SHOCK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507039010/	Quick Look
210	VELA PWN N1	128.8231	-44.9507	128.399065	-44.776941	153.1311	-60.168643	263.36545364	-2.659461	324.0013	56108.9552083333	2012-06-30 22:55:30	56109.3487962963	2012-07-01 08:22:16	507048010	17.8014	15	17.8094	17.8014	0	17.8094	1	1	0	1	1	0	0	19.2047	19.2047	33.9999	1	PROCESSED	57606.5230439815	2016-08-06 12:33:11	56592	2013-10-27 00:00:00	56226.6327083333	2012-10-26 15:11:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070103	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	7	AO7	HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507048010/	Quick Look
211	VELA PWN N2	128.845	-44.6374	128.418547	-44.463562	152.844801	-59.889474	263.12360018	-2.45940596	325.4993	56109.3500115741	2012-07-01 08:24:01	56109.7210185185	2012-07-01 17:18:16	507049010	18.4118	15	18.4198	18.4118	0	18.4198	1	1	0	1	1	0	0	18.7623	18.7623	32.024	0	PROCESSED	57606.5242939815	2016-08-06 12:34:59	56493	2013-07-20 00:00:00	56127.0941319444	2012-07-19 02:15:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070103	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	7	AO7	HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507049010/	Quick Look
212	VELA PWN N3	128.8419	-44.3423	128.413265	-44.168478	152.550585	-59.63427	262.88578161	-2.28439697	325.9006	56109.7216782407	2012-07-01 17:19:13	56110.0161574074	2012-07-02 00:23:16	507050010	12.3984	15	12.3984	12.3984	0	12.3984	1	1	0	1	1	0	0	13.2454	13.2454	25.4319	1	PROCESSED	57606.5311805556	2016-08-06 12:44:54	56493	2013-07-20 00:00:00	56127.104849537	2012-07-19 02:30:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070103	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	7	AO7	HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507050010/	Quick Look
213	VELA PWN N6	128.8205	-43.4604	128.385504	-43.286672	151.68228	-58.872108	262.17003306	-1.76832201	122.021	56258.4379050926	2012-11-27 10:30:35	56258.805625	2012-11-27 19:20:06	507053010	15.3401	15	15.3481	15.3481	0	15.3401	1	1	0	1	1	0	0	13.9013	13.9013	31.7599	0	PROCESSED	57608.0978819444	2016-08-08 02:20:57	56641	2013-12-15 00:00:00	56275.6586111111	2012-12-14 15:48:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070103	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	7	AO7	HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507053010/	Quick Look
214	G7.6+2.0	268.7973	-21.391	268.047539	-21.383335	268.869887	2.045161	7.58937554	2.00788461	270.4016	56194.0843865741	2012-09-24 02:01:31	56194.4237037037	2012-09-24 10:10:08	507065010	16.521	10	16.529	16.521	0	16.5347	2	2	0	2	1	0	0	12.1603	12.1603	29.3139	2	PROCESSED	57607.1654050926	2016-08-07 03:58:11	56676	2014-01-19 00:00:00	56315.5110069444	2013-01-23 12:15:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072014	We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed.	GALACTIC DIFFUSE EMISSION	5	A	TOBIAS PRINZ		EUR	7	AO7	IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507065010/	Quick Look
215	GRXE_E_2	267.6193	-27.2463	266.835371	-27.232829	267.869305	-3.822869	2.00029183	-0.04392641	105.0002	56366.4085532407	2013-03-15 09:48:19	56368.7772569444	2013-03-17 18:39:15	507069010	103.6873	100	103.6873	103.6873	0	103.6873	2	2	0	2	1	0	0	95.5834	95.5834	204.6259	2	PROCESSED	57610.8702314815	2016-08-10 20:53:08	56018	2012-04-01 00:00:00	56379.6047106482	2013-03-28 14:30:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507069010/	Quick Look
216	GRXE_E_3	267.7634	-27.0307	266.980773	-27.017932	267.994323	-3.605243	2.25114568	-0.04369036	105.0001	56368.7777314815	2013-03-17 18:39:56	56371.1111458333	2013-03-20 02:40:03	507070010	101.1726	100	101.1806	101.1726	0	101.1806	2	2	0	2	1	0	0	103.6028	103.6028	201.5898	0	PROCESSED	57610.8916782407	2016-08-10 21:24:01	56018	2012-04-01 00:00:00	56380.5799768518	2013-03-29 13:55:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507070010/	Quick Look
217	MBM36	238.3612	-4.7913	237.700971	-4.643898	237.207481	15.120143	4.00454082	35.69817373	279.4993	56155.0155787037	2012-08-16 00:22:26	56156.7563425926	2012-08-17 18:09:08	507077010	81.0158	80	81.0158	81.0176	0	81.0176	2	2	0	2	1	0	0	80.3301	80.3301	150.3877	4	PROCESSED	57606.8991782407	2016-08-06 21:34:49	56018	2012-04-01 00:00:00	56170.1653240741	2012-08-31 03:58:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076003	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	7	AO7	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507077010/	Quick Look
218	MBM20	68.9377	-14.6308	68.365051	-14.732172	64.468357	-36.225149	211.4041789	-36.56532035	78.376	56164.0544328704	2012-08-25 01:18:23	56166.3530092593	2012-08-27 08:28:20	507079010	82.8814	80	82.8814	82.8814	0	82.8814	2	2	0	2	1	0	0	73.8668	73.8668	198.5577	2	PROCESSED	57606.9726851852	2016-08-06 23:20:40	56018	2012-04-01 00:00:00	56212.7316087963	2012-10-12 17:33:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076003	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	7	AO7	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507079010/	Quick Look
219	3C 397	286.9092	7.1226	286.301586	7.04303	289.342559	29.434869	41.11337729	-0.33398163	251.9939	56595.6848611111	2013-10-30 16:26:12	56597.9106828704	2013-11-01 21:51:23	508001010	103.5157	100	103.5157	103.5157	0	103.5157	2	2	0	2	1	0	0	98.6753	98.6753	192.2937	2	PROCESSED	57613.2313425926	2016-08-13 05:33:08	57012	2014-12-21 00:00:00	56645.6863541667	2013-12-19 16:28:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080011	3C 397 is a Galactic Supernova remnant (SNR) ,whose X-ray spectrum has prominent Fe K line emission. We analyzed Suzaku AO5 data, it resulted in finding of Fe Lya Line. This is a symptomatic of over-ionized (recombining) plasma. On the other hand, the Fe K line center indicates under-ionized (ionizing) plasma. This means that 3C 397 may consisting of two opposite type of plasma: ionizing and recombining. Such a strange state of plasma is not discovered in any SNR.This discovery will be a key to uncovering a mystery of the origin of recombining plasma. However, we still not detect Fe Radiative recombination continuum (RRC),which is a evidence of recombining plasma. To detect the Fe RRC, we propose 150 ks additional observation of 3C 397.	GALACTIC DIFFUSE EMISSION	5	C	RYUSUKE SUGAWARA		JAP	8	AO8	THE INDICATION OF RECOMBINING PLASMA COEXISTING WITH IONIZING PLASMA IN 3C 397	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508001010/	Quick Look
220	W44_EAST	284.1459	1.2991	283.51111	1.232548	285.500202	23.981686	34.67473844	-0.5521979	254.9985	56583.3375231482	2013-10-18 08:06:02	56584.8897337963	2013-10-19 21:21:13	508004010	58.2965	60	58.3045	58.2965	0	58.3149	3	2	0	3	1	0	0	52.7276	52.7276	134.0958	2	PROCESSED	57613.0782407407	2016-08-13 01:52:40	57004	2014-12-13 00:00:00	56637.6520949074	2013-12-11 15:39:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080012	W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	8	AO8	MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508004010/	Quick Look
221	NW_SRC	221.7499	-1.3162	221.105287	-1.10746	219.72393	14.106437	351.9522425	50.22344256	289.0003	56499.3402430556	2013-07-26 08:09:57	56499.8412037037	2013-07-26 20:11:20	508007010	23.554	20	23.554	23.5554	0	23.554	2	2	0	2	1	0	0	24.103	24.103	43.274	0	PROCESSED	57612.0357986111	2016-08-12 00:51:33	56955	2014-10-25 00:00:00	56587.4553819444	2013-10-22 10:55:45	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080020	Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble.	GALACTIC DIFFUSE EMISSION	5	B	MASAYA TAHARA		JAP	8	AO8	SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508007010/	Quick Look
222	SE_SRC	287.3947	-27.2493	286.61657	-27.330736	285.457559	-4.737737	9.97288902	-15.74410072	84.5985	56404.7026967593	2013-04-22 16:51:53	56405.330775463	2013-04-23 07:56:19	508009010	20.3287	20	20.3287	20.3287	0	20.3287	2	2	0	2	1	0	0	17.5938	17.5938	54.2639	1	PROCESSED	57611.1595833333	2016-08-11 03:49:48	56792	2014-05-15 00:00:00	56425.5555092593	2013-05-13 13:19:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080020	Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble.	GALACTIC DIFFUSE EMISSION	5	B	MASAYA TAHARA		JAP	8	AO8	SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508009010/	Quick Look
223	SE_BGD	288.7458	-25.773	287.977196	-25.860714	286.843449	-3.422342	11.87589948	-16.28754896	81.8427	56405.3324537037	2013-04-23 07:58:44	56405.8329050926	2013-04-23 19:59:23	508010010	20.9653	20	20.9693	20.9653	0	20.9733	2	2	0	2	1	0	0	18.7626	18.7626	43.234	0	PROCESSED	57618.7907291667	2016-08-18 18:58:39	56792	2014-05-15 00:00:00	56425.5426851852	2013-05-13 13:01:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080020	Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble.	GALACTIC DIFFUSE EMISSION	5	B	MASAYA TAHARA		JAP	8	AO8	SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508010010/	Quick Look
224	HESS J1534-571 2	233.1754	-57.1	232.193457	-56.931173	246.039407	-36.679353	323.50919975	-0.81659232	295.9986	56544.0219212963	2013-09-09 00:31:34	56544.6695949074	2013-09-09 16:04:13	508014010	38.9186	40	38.9426	38.9186	0	38.9506	2	2	0	2	1	0	0	36.8565	36.8565	55.9539	0	PROCESSED	57612.5722916667	2016-08-12 13:44:06	56990	2014-11-29 00:00:00	56622.6062268518	2013-11-26 14:32:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080024	Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	8	AO8	RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508014010/	Quick Look
225	HESSJ1858-B	284.4324	2.2013	283.801854	2.133387	285.919657	24.847772	35.60820996	-0.39516335	251.7997	56593.9763310185	2013-10-28 23:25:55	56595.1313541667	2013-10-30 03:09:09	508022010	52.595	50	52.619	52.611	0	52.595	3	2	0	2	1	0	0	49.9941	49.9941	99.7858	2	PROCESSED	57613.1665393518	2016-08-13 03:59:49	56975	2014-11-14 00:00:00	56608.7129166667	2013-11-12 17:06:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080052	HESS J1858+020 is one of the unidentified TeV objects which are candidates for the origin of the cosmic-ray protons. Recently a supernova remnant G35.6-0.4 and molecular clouds were discovered in the vicinity of HESSJ1858+020. The TeV emission may be generated through the interaction between protons accelerated in the SNR and the molecular clouds. However, a star forming region in the cloud was also discovered by an infrared observation, and the region may be responsible for the acceleration of protons. We propose Suzaku observations of HESSJ1858+020 to clarify what particles are the origin of the TeV emission, and to clarify what accelerates the particles.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	8	AO8	DECISION OF PARTICLE ACCELERATION SOURCE OF HESS J1858+020 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508022010/	Quick Look
226	JUPITER	104.0103	23.0994	103.254149	23.165009	102.868934	0.282188	192.60135744	11.26438783	264.454	56763.7225	2014-04-16 17:20:24	56764.0627083333	2014-04-17 01:30:18	508023060	8.8696	160	8.8776	8.8696	0	8.8856	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57614.9524652778	2016-08-14 22:51:33	57212	2015-07-09 00:00:00	56846.5928472222	2014-07-08 14:13:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023060/	Quick Look
227	JUPITER	104.4171	23.0664	103.66133	23.133929	103.244601	0.2859	192.79210183	11.59024455	264.5983	56766.7815972222	2014-04-19 18:45:30	56767.1147916667	2014-04-20 02:45:18	508023100	9.3759	160	9.3839	9.3919	0	9.3759	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57614.9623263889	2016-08-14 23:05:45	57212	2015-07-09 00:00:00	56782.4942824074	2014-05-05 11:51:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023100/	Quick Look
228	VELA JR WEST3	131.773	-46.2743	131.349543	-46.08957	158.06279	-60.232297	265.67717372	-1.83917649	116.21	56620.0804861111	2013-11-24 01:55:54	56620.7320949074	2013-11-24 17:34:13	508038010	34.9611	30	34.9911	34.9611	0	34.9611	1	1	0	1	1	0	0	40.4434	40.4434	56.2959	0	PROCESSED	57613.4017708333	2016-08-13 09:38:33	56995	2014-12-04 00:00:00	56629.6399421296	2013-12-03 15:21:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080082	We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution.	GALACTIC DIFFUSE EMISSION	5	C	HIDETOSHI SANO		JAP	8	AO8	FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508038010/	Quick Look
229	VELA PWN W5	126.0444	-45.2057	125.630533	-45.042674	149.898743	-61.36183	262.42223435	-4.39970467	94.9992	56591.8819560185	2013-10-26 21:10:01	56592.3202777778	2013-10-27 07:41:12	508046010	15.8569	15	15.8729	15.8569	0	15.8809	1	1	0	1	1	0	0	12.7358	12.7358	37.8639	0	PROCESSED	57613.1438657407	2016-08-13 03:27:10	57009	2014-12-18 00:00:00	56643.6567824074	2013-12-17 15:45:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080090	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered.	GALACTIC DIFFUSE EMISSION	5	B	KOJI MORI		JAP	8	AO8	SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508046010/	Quick Look
230	VELA PWN W6	125.6171	-45.2116	125.2045	-45.05026	149.354915	-61.513653	262.25511101	-4.65051542	95.0008	56592.3208912037	2013-10-27 07:42:05	56592.8209722222	2013-10-27 19:42:12	508047010	17.2398	15	17.2478	17.2398	0	17.2398	1	1	0	1	1	0	0	16.2299	16.2299	43.1999	0	PROCESSED	57613.1284606482	2016-08-13 03:04:59	57011	2014-12-20 00:00:00	56645.5849421296	2013-12-19 14:02:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080090	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered.	GALACTIC DIFFUSE EMISSION	5	B	KOJI MORI		JAP	8	AO8	SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508047010/	Quick Look
231	RX J1713 SOUTHEAST	258.9281	-40.015	258.058505	-39.959445	261.147328	-16.912866	347.36958165	-0.95677146	84	56711.6431018518	2014-02-23 15:26:04	56713.2190046296	2014-02-25 05:15:22	508067010	80.0774	80	80.0854	80.0854	0	80.0774	2	2	0	2	1	0	0	74.9291	74.9291	118.0069	0	PROCESSED	57613.9112152778	2016-08-13 21:52:09	57173	2015-05-31 00:00:00	56806.6951851852	2014-05-29 16:41:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081313	Detecting thermal emission and determining the ambient density are the missing keys to constrain hadronic acceleration in X-ray synchrotron-dominated SNRs. In the prototypical CR accelerator RX J1713.7-3946, X-ray thermal emission has been sought for over a decade, without success. Deep Suzaku observations will constrain either the conditions of the ambient medium in which the SNR is evolving, or the SN progenitor type (core-collapse or thermonuclear) and nucleosynthesis yield.	GALACTIC DIFFUSE EMISSION	5	A	FABIO ACERO		USA	8	AO8	STUDY OF THE THERMAL EMISSION IN THE SYNCHROTRON DOMINATED SNR RX J1713.7-3946	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508067010/	Quick Look
232	MBM36-OFF	238.9304	-1.7878	238.282545	-1.642781	237.109098	18.17526	7.39248129	37.0792042	270.0134	56533.8916319444	2013-08-29 21:23:57	56535.9634606482	2013-08-31 23:07:23	508074010	74.1565	80	74.1645	74.1645	0	74.1565	3	2	0	2	1	0	0	64.2521	64.2521	178.982	1	PROCESSED	57612.4561574074	2016-08-12 10:56:52	56970	2014-11-09 00:00:00	56603.6967476852	2013-11-07 16:43:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081322	We propose the observation of three off-cloud targets near the targets of the Solar Wind Charge Exchange (SWCX) Key Project to study the properties of the Diffuse X-ray Background below 1 keV, with particular focus on the characterization of the Galactic Halo. The Key Project targets are at a distance of a few hundreds pc from the Sun and their high density portions shields about 90% of X-rays at the O VII energy, our proposed targets, instead, shield only about 50% of the Galactic Halo emission. The contrast between on- and off-cloud allows us to disentangle the foreground and background emissions. In particular we will focus on the properties of the galactic halo, which dominates the oxygen background emission.	GALACTIC DIFFUSE EMISSION	5	A	EUGENIO URSINO		USA	8	AO8	PROPERTIES OF THE GALACTIC HALO THROUGH SHADOW OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508074010/	Quick Look
233	GRXE_E_1	267.4747	-27.4596	266.689479	-27.445424	267.744238	-4.038324	1.75131157	-0.04310182	105.3995	56726.0649537037	2014-03-10 01:33:32	56728.6459722222	2014-03-12 15:30:12	508075010	103.5331	100	103.5491	103.5331	0	103.5559	3	2	0	2	1	0	0	85.3446	85.3446	222.9818	2	PROCESSED	57614.0622453704	2016-08-14 01:29:38	56383	2013-04-01 00:00:00	56740.8547453704	2014-03-24 20:30:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086001	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	8	AO8	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508075010/	Quick Look
234	LDN1563	75.5195	13.8744	74.812622	13.803125	75.779261	-8.85474	187.14092451	-16.70693442	81.1182	56523.4274768518	2013-08-19 10:15:34	56525.2535648148	2013-08-21 06:05:08	508080010	83.588	80	83.588	83.596	0	83.604	2	2	0	2	1	0	0	79.6741	79.6741	157.7538	2	PROCESSED	57612.368912037	2016-08-12 08:51:14	56383	2013-04-01 00:00:00	56587.8175694445	2013-10-22 19:37:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086002	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	8	AO8	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508080010/	Quick Look
235	W49B	287.7839	9.1153	287.185543	9.031646	290.654077	31.289696	43.2808507	-0.18308455	82.0062	57122.7467013889	2015-04-10 17:55:15	57125.7127777778	2015-04-13 17:06:24	509001010	81.4763	400	81.4763	113.9098	0	113.9162	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.986724537	2016-08-17 23:40:53	56748	2014-04-01 00:00:00	57136.5735300926	2015-04-24 13:45:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090007	W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	9	AO9	DEEP OBSERVATIONS OF W49B	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001010/	Quick Look
236	W49B	287.7843	9.1147	287.18594	9.031044	290.654435	31.289046	43.28050127	-0.18371216	82.0064	57128.6891203704	2015-04-16 16:32:20	57131.6619328704	2015-04-19 15:53:11	509001030	100.9959	400	100.9959	106.4207	0	106.3967	4	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.0043518518	2016-08-18 00:06:16	56748	2014-04-01 00:00:00	57220.3809722222	2015-07-17 09:08:36	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090007	W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	9	AO9	DEEP OBSERVATIONS OF W49B	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001030/	Quick Look
237	G1.9+0.3	267.1939	-27.1714	266.410492	-27.155866	267.488865	-3.754805	1.87009843	0.31910459	104.2133	57099.6072569445	2015-03-18 14:34:27	57101.7854976852	2015-03-20 18:51:07	509003010	92.0313	100	92.0313	97.0859	0	97.0699	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8499189815	2016-08-17 20:23:53	57527	2016-05-19 00:00:00	57160.6404861111	2015-05-18 15:22:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090030	We propose a Suzaku observations of the youngest supernova remnant (SNR) G1.9+0.3. We aim to detect flux increase and spectral hardening of synchrotron X-rays since 2011 when the previous Suzaku observation was performed. The measurement should provide us with important information about the maximum acceleration energy attainable by diffusive shock acceleration in SNRs. Suzaku XIS is the most suitable detector since it has the large effective area even in the hard band up to 10 keV. If X-ray flux increase is significantly larger than that measured in the radio band, we can conclude that maximum acceleration energy is becoming higher at present.	GALACTIC DIFFUSE EMISSION	5	A	TAKAAKI TANAKA	YASUNOBU UCHIYAMA	JAP	9	AO9	MEASUREMENT OF TIME VARIABILITY OF SYNCHROTRON X-RAYS FROM THE YOUNGEST SUPERNOVA REMNANT G1.9+0.3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509003010/	Quick Look
238	VELA PWN GEV5	128.1777	-45.5057	127.759875	-45.334391	152.900781	-60.876983	263.54099229	-3.35509044	120.3003	56987.5594328704	2014-11-26 13:25:35	56987.9009490741	2014-11-26 21:37:22	509015010	16.1889	15	16.1889	16.2127	0	16.1969	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.822025463	2016-08-16 19:43:43	57368	2015-12-12 00:00:00	57002.4333564815	2014-12-11 10:24:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090046	We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	9	AO9	X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509015010/	Quick Look
239	G166.0+4.3_SE	81.6718	42.6436	80.778042	42.601144	83.516564	19.390604	166.37682371	4.1455421	266.8508	57094.5870486111	2015-03-13 14:05:21	57095.305	2015-03-14 07:19:12	509024020	26.0329	27	26.0329	27.3929	0	27.3929	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.780625	2016-08-17 18:44:06	57478	2016-03-31 00:00:00	57108.4092939815	2015-03-27 09:49:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090092	Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation.	GALACTIC DIFFUSE EMISSION	5	A	AKIHIRO TAKATA		JAP	9	AO9	G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509024020/	Quick Look
240	CIZA J1358.9-4750_NE	209.8984	-47.6059	209.108141	-47.363535	225.843523	-32.945776	314.66509294	13.70714471	293.0012	56879.8864467593	2014-08-10 21:16:29	56880.8606481482	2014-08-11 20:39:20	509025010	40.2748	40	40.2828	40.2828	0	40.2748	2	2	0	2	1	0	0	7.7468	7.7468	19.736	0	PROCESSED	57616.4833333333	2016-08-16 11:36:00	57270	2015-09-05 00:00:00	56902.1990972222	2014-09-02 04:46:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090102	Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS.	GALACTIC DIFFUSE EMISSION	5	B	YUICHI KATO		JAP	9	AO9	OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509025010/	Quick Look
241	VERJ2019_P2	305.0647	36.873	304.594845	36.714007	321.75914	54.196272	75.14540231	0.26023113	251.4317	56970.0347453704	2014-11-09 00:50:02	56971.0419097222	2014-11-10 01:00:21	509029010	40.4941	40	40.4941	40.5021	0	40.5021	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7544791667	2016-08-16 18:06:27	57436	2016-02-18 00:00:00	57071.4171527778	2015-02-18 10:00:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090120	The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at elongated TeV gamma-ray emission found by Milagro and recently resolved by VERITAS. Although an energetic pulsar PSR J2021+3651 coincides with one of TeV peaks, most of gamma-ray emission still remains unexplained. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we aim to detect X-ray counterparts, presumably unknown pulsar wind nebulae. Connection with a Wolf-Rayet star and an HII region inside this region, which positionally coincide with the gamma-ray peak, will also be investigated.	GALACTIC DIFFUSE EMISSION	5	C	TSUNEFUMI MIZUNO		JAP	9	AO9	SEARCH FOR TEV ACCELERATORS IN NEARBY STAR-FORMING REGION CYGNUS-X WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509029010/	Quick Look
242	HB9-EAST	75.4362	46.2793	74.514835	46.207153	79.087021	23.389602	160.82107477	2.65100841	76.7663	56929.6809722222	2014-09-29 16:20:36	56930.7918518518	2014-09-30 19:00:16	509033010	51.0581	50	51.0581	51.0581	0	51.0581	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6020949074	2016-08-16 14:27:01	57358	2015-12-02 00:00:00	56986.4031481482	2014-11-25 09:40:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091312	We propose to conduct two pointed observations of the Galactic supernova remnant (SNR) HB9 (G160.9+2.6) with Suzaku. HB9 is a member of the class of Galactic SNRs which are distinguished by their contrasting radio and X-ray morphologies. Prior X-ray observations of HB9 have suggested that the SNR may have a hard component to its X-ray emission, but the true nature of this emission and its origin (a background AGN, intercluster gas associated with the cluster that harbors the AGN or the SNR itself) remains elusive. Our proposed observations will help identify the true nature of the hard emission as well as search for spectral variations (and possible overionization) in the properties of the X-ray emitting plasma associated with the SNR.	GALACTIC DIFFUSE EMISSION	5	A	THOMAS PANNUTI		USA	9	AO9	SUZAKU OBSERVATIONS OF THE GALACTIC SUPERNOVA REMNANT HB9 (G160.9+2.6)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509033010/	Quick Look
243	G93.3+6.9 SE RIM	313.3308	55.275	312.981985	55.084608	352.240038	66.77051	93.30192448	6.7583673	52.5	56812.4202314815	2014-06-04 10:05:08	56814.806412037	2014-06-06 19:21:14	509039010	108.0493	100	108.0493	108.0493	0	108.0493	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.2124074074	2016-08-15 05:05:52	57205	2015-07-02 00:00:00	56835.7633912037	2014-06-27 18:19:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091316	We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN.	GALACTIC DIFFUSE EMISSION	5	C	MICHAEL STAGE		USA	9	AO9	G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509039010/	Quick Look
244	OFF-FIELD3	339.5497	30.5758	338.966926	30.315472	354.778732	35.902508	91.73533627	-24.10496467	65.4693	56819.1115625	2014-06-11 02:40:39	56821.2502199074	2014-06-13 06:00:19	509044010	97.3343	80	97.3343	97.3343	0	97.3343	2	2	0	2	1	0	0	38.618	38.618	77.04	0	PROCESSED	57615.247974537	2016-08-15 05:57:05	56748	2014-04-01 00:00:00	56834.8146527778	2014-06-26 19:33:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091321	Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma.	GALACTIC DIFFUSE EMISSION	5	C	ANJALI GUPTA		USA	9	AO9	CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509044010/	Quick Look
245	FERMI_JET_COCOON_3	314.5039	-35.288	313.721159	-35.481827	306.823334	-17.363917	8.28342789	-40.13197139	258.2411	56980.5600694445	2014-11-19 13:26:30	56980.9689583333	2014-11-19 23:15:18	509049010	18.6742	20	18.6742	18.6742	0	18.6742	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7925347222	2016-08-16 19:01:15	57362	2015-12-06 00:00:00	56995.6103240741	2014-12-04 14:38:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091322	The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way.	GALACTIC DIFFUSE EMISSION	5	C	MATTHEW MILLER		USA	9	AO9	OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509049010/	Quick Look
246	FERMI_JET_COCOON_4	313.0188	-30.9125	312.254939	-31.101111	306.880758	-12.815318	13.57103518	-38.16097703	249.0341	56968.206412037	2014-11-07 04:57:14	56968.8473958333	2014-11-07 20:20:15	509050010	21.6767	20	21.6767	21.8127	0	21.8207	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7496412037	2016-08-16 17:59:29	57358	2015-12-02 00:00:00	56982.4333333333	2014-11-21 10:24:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091322	The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way.	GALACTIC DIFFUSE EMISSION	5	C	MATTHEW MILLER		USA	9	AO9	OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509050010/	Quick Look
247	FERMI_JET_COCOON_6	319.6218	-32.8375	318.863263	-33.048426	311.821395	-16.319347	12.30967968	-44.01160773	252.671	56969.3646296296	2014-11-08 08:45:04	56970.0259375	2014-11-09 00:37:21	509052010	21.3583	20	21.3583	21.3583	0	21.3583	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7516782407	2016-08-16 18:02:25	57358	2015-12-02 00:00:00	56982.4382407407	2014-11-21 10:31:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091322	The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way.	GALACTIC DIFFUSE EMISSION	5	C	MATTHEW MILLER		USA	9	AO9	OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509052010/	Quick Look
248	DIFFUSE1B	201.171	8.6653	200.545653	8.925438	196.184358	16.273856	327.54408522	69.93225444	119.3004	57014.7841898148	2014-12-23 18:49:14	57015.2196759259	2014-12-24 05:16:20	509059010	20.7335	20	20.7335	20.7415	0	20.7335	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.558275463	2016-08-17 13:23:55	57475	2016-03-28 00:00:00	57107.4265162037	2015-03-26 10:14:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091324	In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them.	GALACTIC DIFFUSE EMISSION	5	C	JOEL BREGMAN		USA	9	AO9	UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509059010/	Quick Look
249	3C400.2 SE	294.8215	17.1213	294.25847	17.005668	300.577132	37.964226	53.58084569	-2.4098547	81.5889	56770.9416898148	2014-04-23 22:36:02	56771.4758449074	2014-04-24 11:25:13	509070010	24.9467	20	24.9547	24.9467	0	24.9627	1	1	0	1	1	0	0	22.7494	22.7494	46.1359	0	PROCESSED	57614.9903009259	2016-08-14 23:46:02	57152	2015-05-10 00:00:00	56789.6293865741	2014-05-12 15:06:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092010	Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances.	GALACTIC DIFFUSE EMISSION	5	A	JACCO VINK		EUR	9	AO9	THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509070010/	Quick Look
250	MBM16	49.7701	11.5795	49.086508	11.398432	50.445044	-6.509726	170.60720168	-37.27195697	254.3636	57057.0973726852	2015-02-04 02:20:13	57059.5349421296	2015-02-06 12:50:19	509073020	92.0425	80	92.0425	92.0665	0	92.0665	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6060763889	2016-08-17 14:32:45	56748	2014-04-01 00:00:00	57107.434224537	2015-03-26 10:25:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096001	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	9	AO9	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509073020/	Quick Look
251	VELA JR SE3	133.7724	-47.2478	133.349347	-47.055911	161.448089	-60.302336	267.30006641	-1.40128647	110.0008	56629.9618055556	2013-12-03 23:05:00	56630.5806828704	2013-12-04 13:56:11	508062010	27.3638	25	27.3644	27.3638	0	27.3658	2	2	0	2	1	0	0	21.7141	21.7141	53.4599	1	PROCESSED	57613.4843055556	2016-08-13 11:37:24	57005	2014-12-14 00:00:00	56639.5938888889	2013-12-13 14:15:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080117	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr.	GALACTIC DIFFUSE EMISSION	5	C	TARO FUKUYAMA		JAP	8	AO8	OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR.	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508062010/	Quick Look
252	W51SW	290.8908	14.1062	290.315286	14.008227	295.206632	35.736826	49.1149541	-0.54215584	104.3698	55285.3081944444	2010-03-30 07:23:48	55286.3752314815	2010-03-31 09:00:20	504067010	43.7287	40	43.7287	43.7287	0	43.7287	2	2	0	2	1	0	0	9.8137	9.8137	92.1799	0	PROCESSED	57551.0856597222	2016-06-12 02:03:21	55671	2011-04-20 00:00:00	55302.2468055556	2010-04-16 05:55:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040129	We propose to observe the supernova remnant (SNR) W51C with Suzaku XIS. The thermal energy of plasma in W51C, ~3x10^51ergs, is much larger than typical kinetic energy of supernova and can give a large amount of energy to cosmic-ray acceleration. The SNR interactes with the giant molecler cloud and is expected to emit gamma-rays from cosmic-ray interaction. We search for non-thermal X-ray diffuse emission from electron bremsstrahlung or synchrotron emission of secondary electrons produced by decaying charged pions created by p-p interaction.	GALACTIC DIFFUSE EMISSION	5	C	HIDEAKI KATAGIRI		JAP	4	AO4	ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504067010/	Quick Look
253	GALACTIC_BULGE11	269.3164	-32.1646	268.50059	-32.159293	269.404915	-8.724949	358.50010375	-3.80248777	271.7893	55093.1531365741	2009-09-19 03:40:31	55095.6064699074	2009-09-21 14:33:19	504094010	93.1403	50	93.1403	93.1403	0	93.1403	2	2	0	2	1	0	0	82.9543	82.9543	211.9538	1	PROCESSED	57548.674224537	2016-06-09 16:10:53	54922	2009-04-01 00:00:00	55110.4114236111	2009-10-06 09:52:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504094010/	Quick Look
254	GC_SGR_B_NORTH	266.6958	-28.383	265.90497	-28.365031	267.072823	-4.975469	0.60519276	0.06967717	271.4415	53999.7284837963	2006-09-21 17:29:01	54001.2863425926	2006-09-23 06:52:20	501040010	61.3753	62	61.3913	61.3753	61.3833	61.3913	2	2	2	2	1	0	0	53.867	53.867	134.5818	2	PROCESSED	57535.7042361111	2016-05-27 16:54:06	54735	2008-09-26 00:00:00	54021.2828472222	2006-10-13 06:47:18	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010060	We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	1	AO1	OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501040010/	Quick Look
255	VELA SOUTHWEST 1	126.2671	-48.2152	125.877652	-48.051248	153.532268	-63.870386	264.99036518	-5.99332729	119.5649	55164.9700925926	2009-11-29 23:16:56	55165.818900463	2009-11-30 19:39:13	504063010	32.7331	30	32.7492	32.7331	0	32.7411	3	2	0	2	1	0	0	23.7674	23.7674	73.3099	0	PROCESSED	57549.6219791667	2016-06-10 14:55:39	55546	2010-12-16 00:00:00	55179.268587963	2009-12-14 06:26:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040121	We propose 2 pointing-observations of south western part of Vela supernova remnant. Vela SNR has the largest angular size of 8 degree in diameter, so it is suitable to carry out spatial resolved spectroscopy with Suzaku.	GALACTIC DIFFUSE EMISSION	5	C	JUNKO HIRAGA		JAP	4	AO4	X-RAY STUDY ON THE NEAREST SUPERNOVA REMNANT, VELA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504063010/	Quick Look
256	(L,B)=(-20,0)	276.6688	-11.87	275.969796	-11.90065	276.648122	11.416809	19.56512772	0.0074406	263.6004	56215.5456944444	2012-10-15 13:05:48	56219.7479861111	2012-10-19 17:57:06	507044010	171.8231	200	171.8231	171.8231	0	171.8231	2	2	0	2	1	0	0	147.1192	147.1192	363.0377	4	PROCESSED	57607.9036342593	2016-08-07 21:41:14	56602	2013-11-06 00:00:00	56238.7999884259	2012-11-07 19:11:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070084	We will observe the region at (l,b)=(19.57, 0.0112) to measure spatial and temporal fluctuations of the Galactic Ridge X-ray Emission (GRXE). Measuring these fluctuations is a good test to check the scenarios of point sources and star flare for the GRXE origin. Combined with archival data of XMM-Newton, 200 ks observation of Suzaku makes us able to detect the fluctuations lager than 3% of the GRXE flux. The observation mode of XIS is planed to be a normal clocking mode with no window option.	GALACTIC DIFFUSE EMISSION	5	B	HIDEKI UCHIYAMA		JAP	7	AO7	SUZAKU STUDY OF SPATIAL AND TEMPORAL FLUCTUATIONS IN THE GALACTIC RIDGE X-RAY EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507044010/	Quick Look
257	GC17	267.2896	-29.5968	266.49097	-29.581693	267.620125	-6.178087	359.83441438	-1.00224826	260.2809	54384.0425578704	2007-10-11 01:01:17	54384.480787037	2007-10-11 11:32:20	502005010	20.6035	20	20.6035	20.6035	0	20.6035	2	2	0	2	1	0	0	18.1743	18.1743	37.854	1	PROCESSED	57540.245787037	2016-06-01 05:53:56	54777	2008-11-07 00:00:00	54402.5689583333	2007-10-29 13:39:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502005010/	Quick Look
258	VELA PWN NE2	130.6211	-44.2844	130.186671	-44.103918	154.655956	-58.950029	263.6136326	-1.23809583	141.8635	55917.0080439815	2011-12-22 00:11:35	55917.6126273148	2011-12-22 14:42:11	506042010	18.514	15	18.538	18.514	0	18.514	2	2	0	2	1	0	0	16.8755	16.8755	52.2259	0	PROCESSED	57604.2062962963	2016-08-04 04:57:04	56305	2013-01-13 00:00:00	55937.7869212963	2012-01-11 18:53:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	C	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506042010/	Quick Look
259	SGR C BGD	265.7856	-29.8854	264.98542	-29.862996	266.313646	-6.498142	358.90876565	-0.03691694	81.9998	53789.4522106482	2006-02-23 10:51:11	53789.8349421296	2006-02-23 20:02:19	500019010	13.3073	10	13.3153	13.3153	13.3153	13.3073	2	2	2	2	1	0	0	12.2404	12.2404	33.0639	0	PROCESSED	57533.050462963	2016-05-25 01:12:40	54247	2007-05-27 00:00:00	54041.3629166667	2006-11-02 08:42:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001079	We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI MURAKAMI		JAP	0	SWG	FOSSILS OF THE GALACTIC CENTER ACTIVITY	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500019010/	Quick Look
260	HESS J1356-645 2	208.8016	-64.5041	207.885224	-64.258991	235.51443	-48.210014	309.72820731	-2.47708999	123.7329	56340.1852430556	2013-02-17 04:26:45	56341.4863425926	2013-02-18 11:40:20	507020010	51.2594	50	51.2636	51.2594	0	51.2594	2	2	0	2	1	0	0	45.1505	45.1505	112.4059	2	PROCESSED	57610.6176157407	2016-08-10 14:49:22	56718	2014-03-02 00:00:00	56352.5089930556	2013-03-01 12:12:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070017	Recently, pulsar wind nebulae is focused on one of the electron accelerators in our Galaxy. Especially TeV pulsar wind nebulae are supposed to have a largely extended X-ray emission. Since the X-ray emission is much larger than the size considering the typical electron lifetime, high energy electrons strangely seem to be transferred too fast or without cooling. To study the electron diffusion of young pulsar wind nebula, we propose observations of HESS J1356-645, which is off the Galactic plane and is free from the Galactic ridge X-ray emission.	GALACTIC DIFFUSE EMISSION	5	C	TAKAHISA FUJINAGA		JAP	7	AO7	OFF-PLANE TEV GAMMA-RAY SOURCE HESS J1356-645	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507020010/	Quick Look
261	RXJ1713-3946	257.7765	-39.428	256.912609	-39.366986	260.174712	-16.402181	347.32530765	0.10490445	268.0003	53990.7111689815	2006-09-12 17:04:05	53991.0488888889	2006-09-13 01:10:24	501067010	21.1796	20	21.1876	21.1796	21.1931	21.1956	1	1	1	1	1	0	0	21.9861	21.9861	29.1679	0	PROCESSED	57535.5530902778	2016-05-27 13:16:27	54526	2008-03-01 00:00:00	54020.8250925926	2006-10-12 19:48:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501067010/	Quick Look
262	73P/SW3	17.9545	-9.1915	17.327695	-9.456837	12.929266	-15.523337	138.90931762	-71.42827213	59.4015	53893.8691666667	2006-06-07 20:51:36	53893.9356365741	2006-06-07 22:27:19	500014040	3.236	35	3.236	3.236	3.236	3.236	1	1	1	1	1	0	0	2.4909	2.4909	5.7359	0	PROCESSED	57534.5832407407	2016-05-26 13:59:52	54267	2007-06-16 00:00:00	54052.5308912037	2006-11-13 12:44:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014040/	Quick Look
263	G1.9+0.3	267.1951	-27.1633	266.411742	-27.147772	267.489777	-3.746686	1.87759006	0.32236452	104.4114	55643.1608217593	2011-03-23 03:51:35	55645.2856481482	2011-03-25 06:51:20	505053010	100.9235	100	100.9235	100.9315	0	100.9315	2	2	0	2	1	0	0	83.4251	83.4251	183.5657	1	PROCESSED	57601.3345833333	2016-08-01 08:01:48	56025	2012-04-08 00:00:00	55658.2502546296	2011-04-07 06:00:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050084	We propose to observe the youngest (100yr) SNR G1.9+0.3 with Suzaku for 100 ks. The expected scientific fruits are to reveal the earliest stage of SNR evolution via the time variation of synchrotron emission, and to investigate the nuclear synthesis in the SN explosion via the detection of gamma-ray lines from 44Ti.	GALACTIC DIFFUSE EMISSION	5	A	MOTOHIDE KOKUBUN		JAP	5	AO5	INVESTIGATION OF THE YOUNGEST SNR G1.9+0.3 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505053010/	Quick Look
264	SKY_50.0_-62.4	50.0507	-62.4328	49.819854	-62.612067	354.772614	-72.643934	278.67600391	-47.08169247	281.591	53795.7055671296	2006-03-01 16:56:01	53796.9369675926	2006-03-02 22:29:14	501001010	80.145	80	80.153	80.145	80.153	80.145	2	2	2	2	1	0	0	74.0122	74.0122	106.376	0	PROCESSED	57533.1282638889	2016-05-25 03:04:42	54401	2007-10-28 00:00:00	53905.6164930556	2006-06-19 14:47:45	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011252	We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble.	GALACTIC DIFFUSE EMISSION	5	A	ROBIN SHELTON		USA	1	AO1	SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501001010/	Quick Look
265	GC SOUTH	266.5016	-29.1694	265.705845	-29.150477	266.920624	-5.765664	359.84485124	-0.1935349	265.0006	54004.5960185185	2006-09-26 14:18:16	54007.8925231482	2006-09-29 21:25:14	501008010	129.5773	130	129.5773	129.5773	129.5773	129.5773	2	2	2	2	1	0	0	111.2591	111.2591	284.8038	5	PROCESSED	57535.7712731482	2016-05-27 18:30:38	54744	2008-10-05 00:00:00	54021.0929050926	2006-10-13 02:13:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010044	Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	1	AO1	SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501008010/	Quick Look
266	HESS J1745-303	266.2629	-30.3722	265.459457	-30.352101	266.742769	-6.973282	358.71029443	-0.64354718	263.6011	54015.0950462963	2006-10-07 02:16:52	54016.4300810185	2006-10-08 10:19:19	501010010	50.6707	50	50.6707	50.6707	50.6707	50.6707	1	1	1	1	1	0	0	45.6897	45.6897	115.3119	1	PROCESSED	57535.8009837963	2016-05-27 19:13:25	54526	2008-03-01 00:00:00	54021.698587963	2006-10-13 16:45:58	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010046	So far, the evidence for hadron acceleration up to near the knee energy has not yet obtained. Recent galactic plane survey in the TeV gamma-ray band reveals several new unidentified sources like HESS J1745-303. It is extended, hence likely a supernova remnant. Also it coincides with an EGRET unidentified source (3EG J1744-3011), which may suggest that it is a source of accelerated protons. However, HESS J1745-303 shows rather hard spectrum that cannot be explained by the simplest version of the diffusive shock acceleration model. X-ray study on HESS J1745-303 is necessary for further discussions. We might find that observed data requires modification of the common picture that young supernova remnants are the dominant source of high-energy protons.	GALACTIC DIFFUSE EMISSION	5	A	RYO YAMAZAKI		JAP	1	AO1	X-RAY STUDY ON THE TEV UNIDENTIFIED SOURCE HESS J1745-303	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501010010/	Quick Look
267	CYGNUS_LOOP_P7	312.0838	30.7678	311.566097	30.58216	326.462182	46.307536	73.70103145	-8.0534172	239.9966	54416.1673032407	2007-11-12 04:00:55	54416.7223263889	2007-11-12 17:20:09	501018010	24.1545	22	24.1545	24.1545	0	24.1545	2	2	0	2	1	0	0	18.861	18.861	47.92	0	PROCESSED	57540.4878587963	2016-06-01 11:42:31	54798	2008-11-28 00:00:00	54430.1343287037	2007-11-26 03:13:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501018010/	Quick Look
268	HESS J1825-137	276.5031	-13.6997	275.794781	-13.729527	276.397624	9.596588	17.87105596	-0.70261201	269.3213	54025.8175462963	2006-10-17 19:37:16	54027.1682291667	2006-10-19 04:02:15	501044010	50.293	50	50.293	50.293	50.293	50.293	2	2	2	2	1	0	0	42.9557	42.9557	116.694	1	PROCESSED	57535.8789351852	2016-05-27 21:05:40	54526	2008-03-01 00:00:00	54055.4418634259	2006-11-16 10:36:17	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010073	We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	1	AO1	SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501044010/	Quick Look
269	RXJ1713-3946	257.7744	-39.7271	256.908127	-39.666071	260.20044	-16.700257	347.08325974	-0.07081205	268.0001	53990.3113310185	2006-09-12 07:28:19	53990.7106944444	2006-09-12 17:03:24	501066010	20.9207	20	20.9407	20.9207	20.926	20.9447	2	2	2	2	1	0	0	20.699	20.699	34.504	1	PROCESSED	57535.5600347222	2016-05-27 13:26:27	54526	2008-03-01 00:00:00	54020.8077546296	2006-10-12 19:23:10	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501066010/	Quick Look
270	GALACTIC CENTER	265.5037	-30.2156	264.701457	-30.191826	266.078204	-6.8356	358.49956421	-0.00336241	269.0005	54018.2813541667	2006-10-10 06:45:09	54018.887662037	2006-10-10 21:18:14	501052010	19.2451	20	19.2611	19.2611	19.2531	19.2451	2	2	2	2	1	0	0	16.0462	16.0462	52.3799	1	PROCESSED	57535.818275463	2016-05-27 19:38:19	54735	2008-09-26 00:00:00	54053.5074537037	2006-11-14 12:10:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501052010/	Quick Look
271	SNR G93.3+6.9 S2	312.6887	55.4958	312.345372	55.307685	351.959804	67.182569	93.24230604	7.18061007	40.0056	53905.9701736111	2006-06-19 23:17:03	53906.4293865741	2006-06-20 10:18:19	501081010	16.0092	15	16.0352	16.0272	16.0092	16.0352	2	2	2	2	1	0	0	18.3757	18.3757	39.6679	1	PROCESSED	57534.7256134259	2016-05-26 17:24:53	54401	2007-10-28 00:00:00	53927.314537037	2006-07-11 07:32:56	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501081010/	Quick Look
272	PUP A : SE	126.0128	-43.1802	125.58355	-43.01733	147.904142	-59.590498	260.74447692	-3.25911558	277.1832	53843.3098842593	2006-04-18 07:26:14	53843.8328009259	2006-04-18 19:59:14	501089010	29.7493	30	29.7493	29.8172	29.7652	29.7612	4	2	4	4	1	0	0	22.8867	22.8867	45.174	0	PROCESSED	57533.5119675926	2016-05-25 12:17:14	54401	2007-10-28 00:00:00	53907.001412037	2006-06-21 00:02:02	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501089010/	Quick Look
273	MBM12 OFF-CLOUD	41.3205	18.3346	40.61976	18.124407	44.482795	2.251416	157.33933963	-36.81758445	247.4802	53772.648599537	2006-02-06 15:33:59	53774.618275463	2006-02-08 14:50:19	501104010	75.3292	70	75.3372	75.3292	75.3372	75.3372	2	2	2	2	1	0	0	67.769	67.769	170.1159	1	PROCESSED	57532.9691550926	2016-05-24 23:15:35	54401	2007-10-28 00:00:00	53905.9757523148	2006-06-19 23:25:05	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011262	Suzaku will observe MBM 12, a nearby molecular cloud which shadows all but the most local soft X-ray emission. The goal of that observation is to measure the O VII and O VIII emission from the Local Hot Bubble, taking advantage of Suzaku's low energy sensitivity and low background. In light of this, we propose to observe the diffuse background near the MBM 12 position. This will: (1) Measure the O VII and O VIII emission from the Galactic disk and halo, after subtracting the local emission, and (2) confirm that this background emission does not contaminate the initial observation. The absolute measure of the strength of the O VII line, as well as the O VIII/O VII ratio, is essential to understanding the origin of the Galactic component to the 3/4 keV diffuse emission.	GALACTIC DIFFUSE EMISSION	5	B	RANDALL SMITH		USA	1	AO1	THE ORIGIN OF THE GALACTIC DIFFUSE 3/4 KEV X-RAY BACKGROUND	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501104010/	Quick Look
274	MBM16	49.752	11.6015	49.068335	11.420365	50.433531	-6.483887	170.57212752	-37.26756171	73.5786	56139.0841666667	2012-07-31 02:01:12	56140.9710416667	2012-08-01 23:18:18	507076010	24.9499	80	24.9499	24.9499	0	24.9499	2	2	0	2	1	0	0	18.2376	18.2376	162.962	1	PROCESSED	57606.7578703704	2016-08-06 18:11:20	56018	2012-04-01 00:00:00	56260.533125	2012-11-29 12:47:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076003	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	7	AO7	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507076010/	Quick Look
275	VELA JR P9	133.4161	-45.7633	132.983285	-45.572688	159.43463	-59.191033	266.00615013	-0.63304204	347.0009	54287.7015856482	2007-07-06 16:50:17	54287.9516666667	2007-07-06 22:50:24	502031010	13.2524	10	13.2684	13.2524	0	13.2684	1	1	0	1	1	0	0	9.8877	9.8877	21.5999	0	PROCESSED	57539.1152546296	2016-05-31 02:45:58	54703	2008-08-25 00:00:00	54333.4413657407	2007-08-21 10:35:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502031010/	Quick Look
276	VELA JR P5	132.9105	-45.488	132.477402	-45.299188	158.564821	-59.145564	265.56829981	-0.72857938	347.002	54286.4486458333	2007-07-05 10:46:03	54286.7502777778	2007-07-05 18:00:24	502027010	10.977	10	10.977	10.977	0	10.977	1	1	0	1	1	0	0	10.7858	10.7858	26.0539	0	PROCESSED	57539.1013541667	2016-05-31 02:25:57	54696	2008-08-18 00:00:00	54328.4697800926	2007-08-16 11:16:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502027010/	Quick Look
277	VELA JR P12	132.2515	-46.051	131.824752	-45.864543	158.385677	-59.866647	265.71195175	-1.4410688	347.0011	54289.0722106482	2007-07-08 01:43:59	54289.4078009259	2007-07-08 09:47:14	502034010	9.9479	10	9.9479	9.9479	0	9.9479	1	1	0	1	1	0	0	10.494	10.494	28.9839	0	PROCESSED	57539.1227546296	2016-05-31 02:56:46	54696	2008-08-18 00:00:00	54328.4792939815	2007-08-16 11:30:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502034010/	Quick Look
278	HE FOCUSING CONE	49.5833	10.9603	48.902196	10.778547	50.105188	-7.060313	170.9618047	-37.8533007	73.6953	55410.7011921296	2010-08-02 16:49:43	55413.1439699074	2010-08-05 03:27:19	505061010	101.9651	100	101.9731	101.9731	0	101.9651	2	2	0	2	1	0	0	89.1452	89.1452	211.0459	2	PROCESSED	57552.9158796296	2016-06-13 21:58:52	55808	2011-09-04 00:00:00	55441.4075694444	2010-09-02 09:46:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050129	We propose the observation though the Helium Focusng Cone. This region seems to make the strong enhancement of Solarwind Charge exchange and cause the annual variation of it. We develop the best observation of the cone by using the area where the abosorption by molecular cloud is huge. By this observation, we investigate the mistery of the emission of Our Galaxy.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI YOSHITAKE		JAP	5	AO5	OBSERVATION THROUGH THE HELIUM FOCUSING CONE: SEARCH FOR THE VARIABILITY OF THE HELIOSPHERIC SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505061010/	Quick Look
279	VELA JR P17	133.087	-46.0455	132.657371	-45.856052	159.351353	-59.55196	266.0760896	-0.98967894	347.0002	54291.7369444444	2007-07-10 17:41:12	54291.9238773148	2007-07-10 22:10:23	502039010	13.0326	10	13.0645	13.0646	0	13.0326	1	1	0	1	1	0	0	8.8272	8.8272	16.1439	0	PROCESSED	57539.1455555556	2016-05-31 03:29:36	54707	2008-08-29 00:00:00	54333.4040277778	2007-08-21 09:41:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502039010/	Quick Look
280	GC_G0.9+0.1	266.9332	-28.1474	266.1438	-28.130586	267.277369	-4.735296	0.91503767	0.01290063	105.8953	54536.2637152778	2008-03-11 06:19:45	54540.229375	2008-03-15 05:30:18	502051010	138.7614	133	138.7614	138.7614	0	138.7614	2	2	0	2	1	0	0	122.2214	122.2214	342.5768	1	PROCESSED	57541.9299305556	2016-06-02 22:19:06	54919	2009-03-29 00:00:00	54550.6988078704	2008-03-25 16:46:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020071	The Suzaku PV observations found that the diffuse X-rays (6.7 and 6.9 keV-lines) from the GC region can well be explained by a thermal emission from hot plasma (6-7 keV). The most plausible energy injection source is multiple SNe. The huge thermal energy (10^54 ergs) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm this scenario, we propose to observe the shell of G0.9+0.1 and the connecting region of Sgr B and D. The first objective is to detect a thermal emission from the shell of G0.9+0.1 and the second is to discover new SNRs.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	2	AO2	SNR G0.9+0.1 AND THE CONNECTING REGION OF SGR B AND D	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502051010/	Quick Look
281	M17 EAST	275.3895	-16.2062	274.668063	-16.230609	275.205572	7.137102	15.15230897	-0.92571433	271.9996	54377.3569907407	2007-10-04 08:34:04	54380.0940277778	2007-10-07 02:15:24	502052010	114.5695	107	114.5775	114.5695	0	114.5775	2	2	0	2	1	0	0	100.8873	100.8873	236.4498	3	PROCESSED	57540.2317939815	2016-06-01 05:33:47	54771	2008-11-01 00:00:00	54403.5436111111	2007-10-30 13:02:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020085	We continue our XIS study of the soft extended X-ray emission in M17. The first study conducted in a region close to the OB association brought a detailed surface brightness distribution and the highest S/N ratio spectrum of the diffuse emission. In this proposed study, we move our eyes to the west to observe another bright emission outside of the previously studied regions. DSS and ROSAT all-sky survey images suggest that this is a shocked region, in which OB stellar winds impinge upon ISM. We aim to obtain the surface brightness map of this region and measure the plasma temperature difference in and out of the possible shocked region.	GALACTIC DIFFUSE EMISSION	5	A	MASAHIRO TSUJIMOTO		JAP	2	AO2	FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS -	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502052010/	Quick Look
282	VELA JR P32	133.3695	-46.8865	132.945153	-46.696038	160.585523	-60.152729	266.8467839	-1.37881435	347.0018	54655.3279166667	2008-07-08 07:52:12	54655.5648032407	2008-07-08 13:33:19	503044010	11.2649	10	11.2729	11.2649	0	11.2809	1	1	0	1	1	0	0	8.3375	8.3375	20.4559	0	PROCESSED	57543.0006828704	2016-06-04 00:00:59	55048	2009-08-05 00:00:00	54679.381087963	2008-08-01 09:08:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503044010/	Quick Look
283	COMET_8P_TUTTLE-P2_01	39.6412	-35.6843	39.127956	-35.899537	21.259605	-47.847912	240.18300744	-65.68930545	257.5577	54490.0082291667	2008-01-25 00:11:51	54490.1627083333	2008-01-25 03:54:18	502063010	4.3468	5	4.3468	4.3468	0	4.3468	2	2	0	2	1	0	0	4.4029	4.4029	13.3279	1	PROCESSED	57541.3739236111	2016-06-02 08:58:27	54912	2009-03-22 00:00:00	54546.0974189815	2008-03-21 02:20:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063010/	Quick Look
284	COMET_8P_TUTTLE-P2_06	39.9457	-36.3936	39.436659	-36.607889	21.099638	-48.591179	241.70384829	-65.28238509	258.0349	54490.6963773148	2008-01-25 16:42:47	54490.8293287037	2008-01-25 19:54:14	502063060	6.6904	6.7	6.6906	6.6906	0	6.6904	1	1	0	1	1	0	0	4.338	4.338	11.4799	0	PROCESSED	57541.3927893518	2016-06-02 09:25:37	54912	2009-03-22 00:00:00	54546.1201736111	2008-03-21 02:53:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063060/	Quick Look
285	G332.5-5.6 NE	251.0925	-54.3783	250.085838	-54.28574	257.162856	-31.775018	332.77088512	-5.61037777	77.916	54504.4521296296	2008-02-08 10:51:04	54505.6669444444	2008-02-09 16:00:24	502067010	71.1926	80	71.2006	71.2086	0	71.1926	2	2	0	2	1	0	0	65.2508	65.2508	104.9418	0	PROCESSED	57541.5340277778	2016-06-02 12:49:00	54883	2009-02-21 00:00:00	54515.6965509259	2008-02-19 16:43:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021216	We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova.	GALACTIC DIFFUSE EMISSION	5	B	STEPHEN REYNOLDS		USA	2	AO2	G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502067010/	Quick Look
286	GC_LARGEPROJECT6	266.2992	-29.9408	265.498546	-29.920884	266.763082	-6.541223	359.09468885	-0.44519015	265.9621	54723.8160532407	2008-09-14 19:35:07	54725.0348842593	2008-09-16 00:50:14	503012010	57.6855	50	57.6935	57.6855	0	57.6981	2	2	0	2	1	0	0	51.9032	51.9032	105.2878	1	PROCESSED	57543.8433217593	2016-06-04 20:14:23	54557	2008-04-01 00:00:00	54780.6521643518	2008-11-10 15:39:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503012010/	Quick Look
287	HESS_J1825-137_3	276.1966	-13.9971	275.486722	-14.025442	276.082794	9.312755	17.46909054	-0.57831059	271.0001	54758.195775463	2008-10-19 04:41:55	54759.7917476852	2008-10-20 19:00:07	503030010	55.4996	50	55.4996	55.4996	0	55.4996	2	2	0	2	1	0	0	47.3252	47.3252	137.8379	1	PROCESSED	57544.2257407407	2016-06-05 05:25:04	55148	2009-11-13 00:00:00	54780.7804050926	2008-11-10 18:43:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030044	The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons.	GALACTIC DIFFUSE EMISSION	5	B	TAKAAKI TANAKA		JAP	3	AO3	MAPPING OBSERVATIONS OF HESS J1825-137	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503030010/	Quick Look
288	HESS J1804-216	271.1693	-21.6722	270.417896	-21.676057	271.077547	1.764239	8.44223916	-0.04647489	89.0483	53831.6120138889	2006-04-06 14:41:18	53832.4919328704	2006-04-07 11:48:23	500007010	37.5222	50	37.5222	37.5222	37.5222	37.5222	2	2	2	2	1	0	0	28.9336	28.9336	75.9901	0	PROCESSED	57533.4045138889	2016-05-25 09:42:30	54247	2007-05-27 00:00:00	54042.288900463	2006-11-03 06:56:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001029	HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	0	SWG	SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS''	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500007010/	Quick Look
289	HESS J1804-216 BGD	270.9564	-22.0176	270.203045	-22.020418	270.877317	1.420312	8.04431311	-0.04388906	89.2004	53832.4925462963	2006-04-07 11:49:16	53833.454375	2006-04-08 10:54:18	500008010	40.7171	50	40.7171	40.7171	40.7171	40.7171	2	2	2	2	1	0	0	30.6429	30.6429	83.0879	1	PROCESSED	57533.4349537037	2016-05-25 10:26:20	54247	2007-05-27 00:00:00	54056.4266666667	2006-11-17 10:14:24	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001029	HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	0	SWG	SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS''	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500008010/	Quick Look
290	RXJ_0852-4622_NW	132.2926	-45.6157	131.862494	-45.429101	157.976747	-59.482382	265.39238743	-1.14402175	137.763	53723.4478240741	2005-12-19 10:44:52	53727.3016666667	2005-12-23 07:14:24	500010010	175.453	150	175.453	175.525	175.4608	175.461	2	2	2	2	1	0	0	230.0025	230.0025	332.9437	7	PROCESSED	57532.5654513889	2016-05-24 13:34:15	54247	2007-05-27 00:00:00	54059.902662037	2006-11-20 21:39:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001048	We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		JAP	0	SWG	HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500010010/	Quick Look
291	SMC DIFFUSE 1	13.0188	-72.8206	12.579325	-73.092182	312.037754	-64.558836	302.86615918	-44.30756989	221.6864	53687.4452893518	2005-11-13 10:41:13	53688.2231944445	2005-11-14 05:21:24	500011010	46.7789	50	46.7789	46.7869	46.7869	46.7869	1	1	1	1	1	0	0	47.8684	47.8684	67.1999	0	PROCESSED	57527.967337963	2016-05-19 23:12:58	54247	2007-05-27 00:00:00	54038.3531712963	2006-10-30 08:28:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001049	We propose to use Suzaku XIS to observe regions of diffuse emission in the Magellanic Clouds. The diffuse component was identified by ROSAT PSPC observations, but has never been studied with a true spectroscopic instrument. Suzaku is well-matched to the angular size and expected temperature of the regions of diffuse emission in the LMC. Not only will such observations give a clear view of the temperature structure of this gas, they will provide a direct measurement of ambient abundances in the Clouds.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		JAP	0	SWG	DIFFUSE EMISSION IN THE MAGELLANIC CLOUDS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500011010/	Quick Look
292	73P/SW3	18.4857	-9.3839	17.859598	-9.648443	13.351737	-15.906108	140.65827116	-71.47693301	59.4008	53893.6903703704	2006-06-07 16:34:08	53893.7356365741	2006-06-07 17:39:19	500014010	3.228	35	3.228	3.228	3.228	3.228	1	1	1	1	1	0	0	3.312	3.312	3.9039	0	PROCESSED	57534.5195486111	2016-05-26 12:28:09	54267	2007-06-16 00:00:00	54052.5070949074	2006-11-13 12:10:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014010/	Quick Look
293	73P/SW3	18.2949	-9.3163	17.668546	-9.581131	13.199293	-15.770045	140.03044964	-71.46265703	59.3979	53894.3358101852	2006-06-08 08:03:34	53894.4022800926	2006-06-08 09:39:17	500014110	1.4249	35	1.4249	1.4249	1.4249	1.4249	1	1	1	1	1	0	0	1.433	1.433	5.742	0	PROCESSED	57534.5994444445	2016-05-26 14:23:12	54267	2007-06-16 00:00:00	54052.5225694444	2006-11-13 12:32:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014110/	Quick Look
294	HESS J1800-240A	270.4845	-23.9659	269.719972	-23.966397	270.433159	-0.525758	6.13495239	-0.62617494	86.9255	54558.6209606482	2008-04-02 14:54:11	54559.3266087963	2008-04-03 07:50:19	503025010	34.7822	30	34.7822	34.7902	0	34.7902	2	2	0	2	1	0	0	25.7033	25.7033	60.9679	0	PROCESSED	57542.0259837963	2016-06-03 00:37:25	54953	2009-05-02 00:00:00	54574.0504861111	2008-04-18 01:12:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030043	H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region.	GALACTIC DIFFUSE EMISSION	5	A	TAKAAKI TANAKA		JAP	3	AO3	OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503025010/	Quick Look
295	HESS J1800-240C	269.7173	-24.0469	268.95232	-24.043667	269.732245	-0.606264	5.71665641	-0.05804766	87.3071	54563.0147337963	2008-04-07 00:21:13	54563.6877662037	2008-04-07 16:30:23	503027010	30.9755	30	30.9755	30.9755	0	30.9755	2	2	0	2	1	0	0	27.8155	27.8155	58.1239	1	PROCESSED	57542.2510185185	2016-06-03 06:01:28	54953	2009-05-02 00:00:00	54580.1897453704	2008-04-24 04:33:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030043	H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region.	GALACTIC DIFFUSE EMISSION	5	A	TAKAAKI TANAKA		JAP	3	AO3	OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503027010/	Quick Look
296	73P/SW3	18.4874	-9.3902	17.861309	-9.65474	13.350771	-15.912562	140.66879726	-71.4825298	59.4036	53894.6018055556	2006-06-08 14:26:36	53894.680775463	2006-06-08 16:20:19	500014150	3.232	35	3.232	3.232	3.232	3.232	1	1	1	1	1	0	0	3.293	3.293	6.8159	0	PROCESSED	57534.6057638889	2016-05-26 14:32:18	54267	2007-06-16 00:00:00	54052.5265509259	2006-11-13 12:38:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014150/	Quick Look
297	VELA JR P23	132.7881	-46.3947	132.362089	-46.206312	159.378374	-59.957558	266.21323714	-1.3716571	347.0013	54652.3896759259	2008-07-05 09:21:08	54652.7710416667	2008-07-05 18:30:18	503035010	15.6901	10	15.6981	15.6901	0	15.7061	1	1	0	1	1	0	0	11.039	11.039	32.9439	1	PROCESSED	57542.9759490741	2016-06-03 23:25:22	55031	2009-07-19 00:00:00	54664.7904513889	2008-07-17 18:58:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503035010/	Quick Look
298	VELA JR P35	132.966	-46.9473	132.543542	-46.75827	160.188354	-60.35477	266.71715615	-1.62954887	347.0008	54656.2642592593	2008-07-09 06:20:32	54656.5141087963	2008-07-09 12:20:19	503047010	11.5621	10	11.5861	11.5621	0	11.5941	1	1	0	1	1	0	0	9.6198	9.6198	21.5839	0	PROCESSED	57543.0120486111	2016-06-04 00:17:21	55037	2009-07-25 00:00:00	54670.2319212963	2008-07-23 05:33:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503047010/	Quick Look
299	CYGNUS LOOP NE3	313.7583	32.1826	313.244151	31.990973	329.188805	47.043725	75.71932756	-8.27611719	222.9011	53703.7415162037	2005-11-29 17:47:47	53704.2355208333	2005-11-30 05:39:09	500022010	21.1338	20	21.1916	21.7199	21.1338	21.3599	2	2	2	2	1	0	0	20.2445	20.2445	42.6799	1	PROCESSED	57528.1127893518	2016-05-20 02:42:25	54247	2007-05-27 00:00:00	54038.7522106482	2006-10-30 18:03:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001093	We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	0	SWG	CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500022010/	Quick Look
300	HIGH LAT. DIFFUSE A	246.1745	43.4846	245.775383	43.597905	228.822222	63.555652	68.4171583	44.39202319	129.9994	53780.2926388889	2006-02-14 07:01:24	53781.9640509259	2006-02-15 23:08:14	500027010	73.5787	70	73.5867	73.5867	73.5787	73.5867	2	2	2	2	1	0	0	67.3993	67.3993	144.3979	3	PROCESSED	57533.0379976852	2016-05-25 00:54:43	54247	2007-05-27 00:00:00	54041.3110416667	2006-11-02 07:27:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000044	We propose observing the diffse background at two locations where the low temperature component is particularly string. One of the these enhancement is ostensibly an extension of the local bubble, while the other it is probably due to a region of very bright emission in the halo (z> 400 pc). We can verify the thermal nature of these sources, and look for CNO abyndance ratio differences between local disk and halo gas. It is critical to make these abundance determinations before the low energy response deteriorates any further. Note that this observation should also allow a calibration of the XIS response below the carbon edge to ~20%.	GALACTIC DIFFUSE EMISSION	5	A	SWG		JAP	0	SWG	HIGH LATTITUDE DIFFUSE A & B	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500027010/	Quick Look
301	GALACTIC CENTER	266.0341	-30.1068	265.232432	-30.085596	266.53657	-6.713302	358.83318764	-0.33628911	269.0002	54019.4218402778	2006-10-11 10:07:27	54020.1446064815	2006-10-12 03:28:14	501057010	20.4884	20	20.4884	20.4964	20.4964	20.4964	2	2	2	2	1	0	0	19.086	19.086	62.4379	0	PROCESSED	57535.8262037037	2016-05-27 19:49:44	54735	2008-09-26 00:00:00	54053.6059837963	2006-11-14 14:32:37	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501057010/	Quick Look
302	SKY_53.3_-63.4	53.24	-63.4549	53.047022	-63.62196	354.144887	-74.40934	278.62179386	-45.30780651	286.1724	53797.8694444444	2006-03-03 20:52:00	53800.3342476852	2006-03-06 08:01:19	501002010	101.4752	100	101.4752	101.4752	101.4752	101.4752	2	2	2	2	1	0	0	145.4318	145.4318	212.8539	4	PROCESSED	57533.1863425926	2016-05-25 04:28:20	54401	2007-10-28 00:00:00	53906.7729282407	2006-06-20 18:33:01	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011252	We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble.	GALACTIC DIFFUSE EMISSION	5	A	ROBIN SHELTON		USA	1	AO1	SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501002010/	Quick Look
303	CYGNUS LOOP (P26)	314.1252	30.3135	313.601346	30.1206	328.529731	45.204244	74.46090737	-9.70687059	49.7995	54599.1203587963	2008-05-13 02:53:19	54599.5474421296	2008-05-13 13:08:19	503062010	16.9247	15	16.9247	16.9327	0	16.9327	2	2	0	2	1	0	0	15.441	15.441	36.892	1	PROCESSED	57542.5181944444	2016-06-03 12:26:12	54975	2009-05-24 00:00:00	54609.1293981482	2008-05-23 03:06:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503062010/	Quick Look
304	GC SOUTH BGD	266.1893	-28.9082	265.395265	-28.887768	266.639666	-5.511508	359.92534776	0.17564926	265.0003	54007.8931365741	2006-09-29 21:26:07	54009.2884143518	2006-10-01 06:55:19	501009010	51.19	50	51.198	51.206	51.19	51.198	2	2	2	2	1	0	0	47.7157	47.7157	120.5479	0	PROCESSED	57535.7087847222	2016-05-27 17:00:39	54735	2008-09-26 00:00:00	54020.9371064815	2006-10-12 22:29:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010044	Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	1	AO1	SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501009010/	Quick Look
305	G344.7-0.1	255.9588	-41.7032	255.078113	-41.633558	258.959028	-18.797881	344.67682908	-0.15577285	89.2821	54152.1890393518	2007-02-21 04:32:13	54153.2919097222	2007-02-22 07:00:21	501011010	42.1336	40	42.1336	42.1336	0	42.1336	2	2	0	2	1	0	0	34.2016	34.2016	95.28	1	PROCESSED	57537.4329050926	2016-05-29 10:23:23	54777	2008-11-07 00:00:00	54158.2352662037	2007-02-27 05:38:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010050	We propose an observation of a supernova remnant (SNR) G344.7-0.1 with Suzaku. In addition to emission lines from highly ionized ions (Si, S, and so on), we found a strong emission line at 6.4 keV in the spectra obtained with ASCA and XMM-Newton. This line is thought to be a K-line from the low-ionized Fe, but the origin is still unknown. Precise measurements of the line energy and the spectral parameters with the XIS will provide us with understanding the origin of the Fe-K line and the physical process in the SNR.	GALACTIC DIFFUSE EMISSION	5	C	SHIGEO YAMAUCHI		JAP	1	AO1	SUZAKU OBSERVATION OF G344.7-0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501011010/	Quick Look
306	CYGNUS_LOOP_P13	313.4901	31.0708	312.971102	30.880128	328.238327	46.115492	74.70349314	-8.80441033	68.2467	53865.1416666667	2006-05-10 03:24:00	53865.5321643518	2006-05-10 12:46:19	501030010	17.073	17	17.073	17.081	17.089	17.089	1	1	1	1	1	0	0	14.269	14.269	33.7279	0	PROCESSED	57534.2605092593	2016-05-26 06:15:08	54394	2007-10-21 00:00:00	53914.0847569444	2006-06-28 02:02:03	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501030010/	Quick Look
307	CAS A	351.0231	59.0265	350.456601	58.751794	27.744986	54.948342	111.88943817	-1.95981315	208.1115	54876.0965740741	2009-02-14 02:19:04	54876.8363310185	2009-02-14 20:04:19	503080010	30.0355	30	30.0355	30.0355	0	30.0355	2	2	0	2	1	0	0	30.0731	30.0731	63.9139	0	PROCESSED	57545.551087963	2016-06-06 13:13:34	55330	2010-05-14 00:00:00	54892.9889699074	2009-03-02 23:44:07	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030127	Cas A is the youngest supernova remnant(SNR) in our Galaxy. Recently, the Spitzer Space Telescope discovered moving structures nearly at the speed of light outside the shell of the SNR. These structures are likely infrared echoes, where interstellar dust is heated by the outward moving photon shell of a bright flash. The bright flash is probably due to a giant flare from the central point source of Cas A, and if so, it requires that the central point source is a magnetar. Magnetars are known to emit luminous flares in the X-ray band, so it is expected that we can detect Fe-K fluorescence emission accompanied by IR echo. Here, we propose to observe on IR-emitting cloud around Cas A for 30ks to search for Fe-K emission which is naturally expected if the central point source is a magnetar.	GALACTIC DIFFUSE EMISSION	5	C	HIROYUKI AONO		JAP	3	AO3	INVESTIGATION OF A X-RAY ECHO NEAR THE SUPERNOVA REMNANT CASSIOPEIA A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503080010/	Quick Look
308	G156.2+5.7E	75.8128	51.6405	74.832405	51.569986	80.017374	28.69124	156.70319129	6.10796494	274.6638	54149.9177893518	2007-02-18 22:01:37	54151.1750231482	2007-02-20 04:12:02	501074010	53.3331	50	53.3494	53.3491	0	53.3331	2	2	0	2	1	0	0	50.8218	50.8218	108.6199	2	PROCESSED	57537.4302893518	2016-05-29 10:19:37	54773	2008-11-03 00:00:00	54158.2839583333	2007-02-27 06:48:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011235	G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target.	GALACTIC DIFFUSE EMISSION	5	C	ROBERT PETRE		USA	1	AO1	A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501074010/	Quick Look
309	SNR G93.3+6.9 S3	313.171	55.2801	312.823004	55.090273	352.082126	66.837166	93.24775568	6.83197363	40.0152	53906.4300462963	2006-06-20 10:19:16	53906.7266087963	2006-06-20 17:26:19	501082010	16.3347	15	16.3347	16.3587	16.3507	16.3427	1	1	1	1	1	0	0	13.9186	13.9186	25.6159	0	PROCESSED	57534.7339814815	2016-05-26 17:36:56	54401	2007-10-28 00:00:00	53926.2481365741	2006-07-10 05:57:19	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501082010/	Quick Look
310	PUP A : NE	125.7583	-42.7117	125.326284	-42.549841	147.156331	-59.259606	260.25284038	-3.14403225	277.1213	53842.913287037	2006-04-17 21:55:08	53843.3091319445	2006-04-18 07:25:09	501087010	20.7109	20	20.7336	20.7349	20.7189	20.7109	1	1	1	1	1	0	0	19.7443	19.7443	34.1899	1	PROCESSED	57533.5127083333	2016-05-25 12:18:18	54401	2007-10-28 00:00:00	53906.9450231482	2006-06-20 22:40:50	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501087010/	Quick Look
311	TYCHO SNR	6.3139	64.1469	5.613879	63.870082	42.846574	53.765969	120.08177164	1.42013769	53.7834	54682.0646759259	2008-08-04 01:33:08	54686.9529398148	2008-08-08 22:52:14	503085010	312.892	400	312.916	312.892	0	312.908	2	2	0	2	1	0	0	289.9494	289.9494	307.8699	3	PROCESSED	57543.3766782407	2016-06-04 09:02:25	54557	2008-04-01 00:00:00	54707.038287037	2008-08-29 00:55:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031003	Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		USA	3	AO3	SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503085010/	Quick Look
312	N11 SB	74.1823	-66.412	74.156384	-66.487992	354.048784	-83.709745	277.1886014	-36.07081942	146.432	54046.4407291667	2006-11-07 10:34:39	54047.232037037	2006-11-08 05:34:08	501091010	30.452	30	30.452	30.452	30.452	30.452	2	2	2	2	1	0	0	26.405	26.405	68.3659	0	PROCESSED	57536.0384953704	2016-05-28 00:55:26	54455	2007-12-21 00:00:00	54088.5643287037	2006-12-19 13:32:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011251	Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 2 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 4 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission.	GALACTIC DIFFUSE EMISSION	5	C	ROSA WILLIAMS		USA	1	AO1	A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501091010/	Quick Look
313	VELA PULSAR/PWN 3	128.6368	-45.8007	128.219858	-45.627635	153.778024	-60.967724	263.96966687	-3.27226783	344.1164	53925.347974537	2006-07-09 08:21:05	53926.0467476852	2006-07-10 01:07:19	501110010	17.5886	20	17.6046	17.5886	17.5886	17.6046	1	1	1	1	1	0	0	17.2252	17.2252	60.3519	0	PROCESSED	57534.8715509259	2016-05-26 20:55:02	54401	2007-10-28 00:00:00	53930.634224537	2006-07-14 15:13:17	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014211	The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band.	GALACTIC DIFFUSE EMISSION	5	B	OLEG KARGALTSEV	KOJI MORI	USJ	1	AO1	THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501110010/	Quick Look
314	B1920+10(2)	292.8971	10.8605	292.305399	10.753499	296.831046	32.19317	47.18977478	-3.80874006	248.6642	54783.7420833333	2008-11-13 17:48:36	54785.8981365741	2008-11-15 21:33:19	503091010	100.4577	100	100.4577	100.4577	0	100.4577	2	2	0	2	1	0	0	93.8731	93.8731	186.248	0	PROCESSED	57544.4390972222	2016-06-05 10:32:18	55167	2009-12-02 00:00:00	54797.1537731482	2008-11-27 03:41:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031204	A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps.	GALACTIC DIFFUSE EMISSION	5	C	ZDENKA MISANOVIC		USA	3	AO3	STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503091010/	Quick Look
315	GCL4	265.3437	-29.192	264.548064	-29.167468	265.905576	-5.816983	359.29532739	0.65531706	106.9407	54907.3257986111	2009-03-17 07:49:09	54908.0711111111	2009-03-18 01:42:24	503102010	33.6554	25	33.6794	33.6558	0	33.6554	2	2	0	2	1	0	0	30.0521	30.0521	64.3899	0	PROCESSED	57545.8492939815	2016-06-06 20:22:59	55329	2010-05-13 00:00:00	54920.054837963	2009-03-30 01:18:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031234	We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity.	GALACTIC DIFFUSE EMISSION	5	B	FARHAD YUSEF-ZADEH		USA	3	AO3	A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503102010/	Quick Look
316	HESS J1745-303 1	266.2249	-30.1096	265.423171	-30.089321	266.702778	-6.71164	358.91712668	-0.478438	70.5005	54527.7555555556	2008-03-02 18:08:00	54529.7363310185	2008-03-04 17:40:19	502016010	70.5291	67	70.5371	70.5291	0	70.5451	2	2	0	2	1	0	0	61.7932	61.7932	171.0959	3	PROCESSED	57541.8000810185	2016-06-02 19:12:07	54908	2009-03-18 00:00:00	54539.3190509259	2008-03-14 07:39:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020023	A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku.	GALACTIC DIFFUSE EMISSION	5	B	RYO YAMAZAKI		JAP	2	AO2	SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502016010/	Quick Look
317	ANTICENTER	113.3357	-19.5305	112.785719	-19.421448	119.46206	-40.613154	234.9976882	0.00424804	280.7829	54212.8606481482	2007-04-22 20:39:20	54215.4197222222	2007-04-25 10:04:24	502021010	89.5429	80	89.5509	89.5589	0	89.5429	2	2	0	2	1	0	0	78.9887	78.9887	221.0508	3	PROCESSED	57538.5236689815	2016-05-30 12:34:05	54744	2008-10-05 00:00:00	54223.2040046296	2007-05-03 04:53:46	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020032	We propose to observe diffuse radiation from the Galactic plane in the general direction of the anticenter. Absolute measurement of the O VII and O VIII line fluxes will help establish the origin of this mysterious component of the diffuse background. This will allow a search for spectral signatures of non-thermal emission, i.e. charge- exchange emission, in the 3/4 keV band and the determination of abundances in hot gas thermal emission without risk of confusion by emission from hot gas in the Galactic Bulge.	GALACTIC DIFFUSE EMISSION	5	B	KENSUKE MASUI		JAP	2	AO2	SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502021010/	Quick Look
318	VELA JR P1	131.9787	-45.8064	131.551046	-45.620931	157.807694	-59.76004	265.40235777	-1.43438498	347.0031	54285.3151273148	2007-07-04 07:33:47	54285.6904398148	2007-07-04 16:34:14	502023010	10.6496	10	10.6496	10.6576	0	10.6576	2	2	0	2	1	0	0	9.0446	9.0446	32.4199	0	PROCESSED	57539.086412037	2016-05-31 02:04:26	54696	2008-08-18 00:00:00	54328.4268402778	2007-08-16 10:14:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502023010/	Quick Look
319	VELA JR P8	133.862	-45.8612	133.428362	-45.669016	160.04869	-59.10729	266.28131071	-0.45847751	347.0005	54287.3028240741	2007-07-06 07:16:04	54287.7009722222	2007-07-06 16:49:24	502030010	13.2196	10	13.2196	13.2196	0	13.2196	2	2	0	2	1	0	0	14.441	14.441	34.3919	0	PROCESSED	57539.112662037	2016-05-31 02:42:14	54703	2008-08-25 00:00:00	54333.4507175926	2007-08-21 10:49:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502030010/	Quick Look
320	VELA JR P13	131.851	-46.106	131.426011	-45.92099	157.974394	-60.061119	265.57984888	-1.69160478	347.0011	54290.1290162037	2007-07-09 03:05:47	54290.4411342593	2007-07-09 10:35:14	502035010	9.4089	10	9.4089	9.4089	0	9.4089	2	2	0	2	1	0	0	8.9531	8.9531	26.9639	0	PROCESSED	57539.1321412037	2016-05-31 03:10:17	54696	2008-08-18 00:00:00	54328.4906134259	2007-08-16 11:46:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502035010/	Quick Look
321	SN1006	225.7268	-41.9424	224.908794	-41.746586	235.456683	-23.661429	327.58003425	14.55159393	117.0193	54521.6264351852	2008-02-25 15:02:04	54526.8613310185	2008-03-01 20:40:19	502046010	211.7373	200	211.7453	211.7373	0	211.7453	2	2	0	2	1	0	0	184.3622	184.3622	417.2759	6	PROCESSED	57541.8622337963	2016-06-02 20:41:37	54904	2009-03-14 00:00:00	54535.729375	2008-03-10 17:30:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020052	Thermal plasma incident SN1006 has very interesting characteristic. Suzaku PV spectrum revealed ionization parameter of the plasma is significantly low. We investigated the spatial variation of the ionization parameter, and found the outer region of SN1006 has lower ionization parameter than the inner region. However, since the center region of SN1006 is placed on the edge of FOV in the PV observation, the spectra have poor statistics, and the ionization state and the metal abundance cannot be decided with good precision. We propose to observe the center region of SN1006 deeply to decide the physical condition of the plasma of young SNR. Necessary exposure time is 150ksec.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		JAP	2	AO2	THE CENTER REGION OF SN1006	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502046010/	Quick Look
322	HESS J1702-420	255.6874	-42.0709	254.803902	-41.999975	258.786548	-19.184424	344.26217794	-0.21974248	106.4451	54550.458599537	2008-03-25 11:00:23	54555.625162037	2008-03-30 15:00:14	502049010	215.6932	200	215.7053	215.6932	0	215.7053	2	2	0	2	1	0	0	140.6375	140.6375	395.7215	6	PROCESSED	57542.1678356482	2016-06-03 04:01:41	54933	2009-04-12 00:00:00	54566.9486458333	2008-04-10 22:46:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020067	The Galactic Plane Survey with HESS found several new TeV sources, called as "dark particle accelerators". They must be powerful cosmic-ray accelerators, although their origin is still unknown due to the lack of information in other wavelengths. We investigate one of the most mysterious sample, HESS J1702-420, which has the brightest HESS compact source without clear counterparts. ASCA Galactic plane survey shows no evidence of X-ray emission although the exposure was too short. With the large effective area and the low background of XISs, we will be able to detect quite dim counterpart or make strong upper-limit in the hard X-ray band. This result will lead us to distinguish that HESS J1702-420 is the true "dark" protonic accelerator, or a hypothetical PWN powered by PSR J1702-4128.	GALACTIC DIFFUSE EMISSION	5	B	AYA BAMBA		JAP	2	AO2	RESOLVING THE DARKEST DARK PARTICLE ACCELERATOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502049010/	Quick Look
323	COMET_8P_TUTTLE-P1-6	28.2017	6.7525	27.54593	6.506397	28.607042	-4.520684	148.82276905	-53.00641332	248.5018	54470.8491666667	2008-01-05 20:22:48	54470.9154050926	2008-01-05 21:58:11	502062060	2.0266	2	2.0266	2.0266	0	2.0266	1	1	0	1	1	0	0	2.044	2.044	5.664	0	PROCESSED	57541.0007986111	2016-06-02 00:01:09	54908	2009-03-18 00:00:00	54542.2318634259	2008-03-17 05:33:53	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062060/	Quick Look
324	COMET_8P_TUTTLE-P2_02	39.704	-35.8295	39.191609	-36.044542	21.228259	-48.000366	240.49763907	-65.60654763	257.6692	54490.1630902778	2008-01-25 03:54:51	54490.2960069444	2008-01-25 07:06:15	502063020	5.2049	5	5.2049	5.2049	0	5.2049	1	1	0	1	1	0	0	5.5919	5.5919	11.4499	0	PROCESSED	57541.3791898148	2016-06-02 09:06:02	54912	2009-03-22 00:00:00	54546.1091666667	2008-03-21 02:37:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063020/	Quick Look
325	COMET_8P_TUTTLE-P2_07	40.0041	-36.5319	39.495887	-36.746007	21.066088	-48.735556	241.99586619	-65.20252382	258.1285	54490.8297106482	2008-01-25 19:54:47	54490.962662037	2008-01-25 23:06:14	502063070	5.2676	5	5.2916	5.2676	0	5.2994	1	1	0	1	1	0	0	2.753	2.753	11.4799	0	PROCESSED	57541.3952777778	2016-06-02 09:29:12	54912	2009-03-22 00:00:00	54546.130462963	2008-03-21 03:07:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063070/	Quick Look
326	COMET_8P_TUTTLE-P2_BGD-2	40.4817	-37.5941	39.980067	-37.806706	20.824934	-49.853115	244.17118034	-64.55380496	254.4101	54492.5631365741	2008-01-27 13:30:55	54492.7293287037	2008-01-27 17:30:14	502064020	6.9797	5	6.9797	7.0037	0	6.9877	1	1	0	1	1	0	0	5.5471	5.5471	14.3519	0	PROCESSED	57554.5355671296	2016-06-15 12:51:13	54912	2009-03-22 00:00:00	54546.2537847222	2008-03-21 06:05:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502064020/	Quick Look
327	G21.5-0.9	278.4035	-10.5067	277.711514	-10.545731	278.460081	12.687392	21.56184596	-0.8687642	103.5554	54188.7945023148	2007-03-29 19:04:05	54189.6252199074	2007-03-30 15:00:19	502065010	25.1416	100	25.156	25.1416	0	25.156	1	2	0	1	1	0	0	22.889	22.889	71.7699	1	PROCESSED	57538.0286921296	2016-05-30 00:41:19	54695	2008-08-17 00:00:00	54209.5181018518	2007-04-19 12:26:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021211	We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray.	GALACTIC DIFFUSE EMISSION	5	B	ILANA HARRUS		USA	2	AO2	SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502065010/	Quick Look
328	G296.1-0.5N	177.8287	-62.3875	177.210977	-62.109277	215.982021	-55.076396	296.02814016	-0.3243747	322.3815	54321.2538541667	2007-08-09 06:05:33	54323.4522453704	2007-08-11 10:51:14	502068010	77.1759	67	77.1759	77.1759	0	77.1759	2	2	0	2	1	0	0	68.4846	68.4846	189.9237	1	PROCESSED	57539.4859953704	2016-05-31 11:39:50	54716	2008-09-07 00:00:00	54347.5137268518	2007-09-04 12:19:46	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021218	Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles.	GALACTIC DIFFUSE EMISSION	5	B	KAZIMIERZ BORKOWSKI		USA	2	AO2	G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502068010/	Quick Look
329	GC CENTER #2	266.7693	-28.6295	265.976908	-28.611884	267.143281	-5.22043	0.42794484	-0.11339991	74.7707	53821.958587963	2006-03-27 23:00:22	53823.7585069444	2006-03-29 18:12:15	500005010	88.4247	100	88.4327	88.4247	88.4327	88.4327	2	2	2	2	1	0	0	64.5911	64.5911	155.5019	2	PROCESSED	57533.3630324074	2016-05-25 08:42:46	54247	2007-05-27 00:00:00	54133.0079861111	2007-02-02 00:11:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001020	We propose to obtain high quality spectrum near the GC. The objective is to resolve 6.4, 6.7, and 6.9 keV line and determine the high energy tail and sub-structures, which may be X-ray reflection from Sgr A* (6.4 keV line + 7.1 keV edge + high energy tail), thermal plasma (6.7 + 6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	0	SWG	SUZAKU GALACTIC CENTER OBSERVATION PROJECT: #2 SGR B1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500005010/	Quick Look
330	HESS J1731-347 SW	263.0074	-34.9458	262.173825	-34.909887	264.142527	-11.646447	353.3803333	-0.77058494	92.6086	55245.72	2010-02-18 17:16:48	55246.5231365741	2010-02-19 12:33:19	504031010	41.8615	40	41.8779	41.8615	0	41.8695	2	2	0	2	1	0	0	34.1028	34.1028	69.382	0	PROCESSED	57550.6419675926	2016-06-11 15:24:26	55623	2011-03-03 00:00:00	55257.0493981482	2010-03-02 01:11:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040026	Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1731-347 is one of only 3 TeV SNRs which have a radio shell and possible thermal X-rays. With good statistics and low background observation of Suzaku XIS, we will detect thermal X-rays from the shell of HESS J1731-347 for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition.	GALACTIC DIFFUSE EMISSION	5	B	AYA BAMBA		JAP	4	AO4	DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504031010/	Quick Look
331	SNR 0049-73.6	12.7817	-73.3677	12.345533	-73.639533	310.812589	-64.728588	302.96274339	-43.76053264	62.7682	54629.4818518518	2008-06-12 11:33:52	54632.7605787037	2008-06-15 18:15:14	503094010	120.478	120	120.486	120.478	0	120.486	2	2	0	2	1	0	0	107.7079	107.7079	283.2419	3	PROCESSED	57542.894525463	2016-06-03 21:28:07	55008	2009-06-26 00:00:00	54642.6050694444	2008-06-25 14:31:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031211	We propose to observe the O-rich supernova remnant (SNR) 0049-73.6 in the Small Magellanic Cloud (SMC). SNR 0049-73.6 shares some similarities and differences with another O-rich SNR 0103-72.6 in the SMC. High resolution X-ray spectroscopy of these SNRs with Suzaku/XIS observations should provide a useful insight for the details of thermal evolution of a core-collapse SNR. We began this program with an AO1 Suzaku/XIS observation of SNR 0103-72.6. We here propose to continue this program with our AO3 Suzaku observation of 0049-73.6. We request for a 120 ks Suzaku/XIS observation of 0049-73.6.	GALACTIC DIFFUSE EMISSION	5	B	SANGWOOK PARK		USA	3	AO3	OXYGEN-RICH SUPERNOVA REMNANT 0049-73.6 IN THE SMC	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503094010/	Quick Look
332	TORNADO	265.1272	-30.949	264.32027	-30.923391	265.775878	-7.579198	357.70572925	-0.11631727	269.1137	55072.5037037037	2009-08-29 12:05:20	55075.0093055556	2009-09-01 00:13:24	504036010	125.0692	120	125.0692	125.0772	0	125.0772	2	2	0	2	1	0	0	97.0913	97.0913	216.4598	3	PROCESSED	57548.5178356482	2016-06-09 12:25:41	55454	2010-09-15 00:00:00	55088.3064814815	2009-09-14 07:21:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040076	The Tornado is an unusual and intense radio source located in the galactic center region. It has a polarized non-thermal radio spectrum. t has very unique morphology of elongated and loop-like structure. However, no crucial observational result determining the nature has been obtained. With the Suzaku AO3 observation of the Tornado (50ks), we found interesting signs of 2.45-keV He like S-K line, diffuse emission from the "tail" and the whole "head". The purpose of this observation is to obtain precise spectrum and spatial distribution. If the thermal S-K line is confirmed and it has a high metal abundance, the nature of the Tornado is an SNR. We also investigate the extreme structure of the tail and search for power-law component in spectra.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	4	AO4	REVEALING THE UNUSUAL SOURCE, THE NATURE OF THE "TORNADO", IN THE GALACTIC CENTER REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504036010/	Quick Look
333	GC_LARGEPROJECT1	266.4387	-28.5683	265.646756	-28.549082	266.850456	-5.166114	0.32941305	0.16640393	260.8767	54711.4273958333	2008-09-02 10:15:27	54712.9530555556	2008-09-03 22:52:24	503007010	52.1523	50	52.1523	52.1523	0	52.1523	2	2	0	2	1	0	0	44.1838	44.1838	131.7938	2	PROCESSED	57543.7627546296	2016-06-04 18:18:22	54557	2008-04-01 00:00:00	54780.6858796296	2008-11-10 16:27:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503007010/	Quick Look
334	GC_LARGEPROJECT11	264.7183	-31.3859	263.908606	-31.358306	265.438625	-8.028238	357.14965021	-0.05250387	268.3335	54732.3390046296	2008-09-23 08:08:10	54733.3897337963	2008-09-24 09:21:13	503017010	51.2865	50	51.2945	51.2865	0	51.3025	2	2	0	2	1	0	0	48.5834	48.5834	90.7759	2	PROCESSED	57543.9868287037	2016-06-04 23:41:02	54557	2008-04-01 00:00:00	54780.6941550926	2008-11-10 16:39:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503017010/	Quick Look
335	LOOP 1 L=356.00	263.2426	-31.9466	262.429689	-31.911872	264.194275	-8.641352	356.00010804	0.70279756	93.3363	54908.96625	2009-03-18 23:11:24	54909.8933333333	2009-03-19 21:26:24	503022010	41.3193	40	41.3193	41.3193	0	41.3193	2	2	0	2	1	0	0	34.3187	34.3187	80.0699	0	PROCESSED	57545.8730671296	2016-06-06 20:57:13	55330	2010-05-14 00:00:00	54923.2640162037	2009-04-02 06:20:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030023	NANTEN telescope discovered huge molecular loops in the galactic center region. The model that the huge loops is due to magnetic buoyancy caused by the Parkey instability is proposed. The loops size is 12 order of magnitude larger than the solar loops, but the physics would be common. X-ray emission from shock heated and/or accelerated particles would be expected at the foot point of the loops. We propose an X-ray observation at the foot point of the molecular loop with Suzaku and investigate the magnetic activity in the galactic scale.	GALACTIC DIFFUSE EMISSION	5	C	SHIGEO YAMAUCHI		JAP	3	AO3	SUZAKU OBSERVATION OF MOLECULAR LOOPS IN THE GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503022010/	Quick Look
336	LOOP 2 L=356.33	263.4562	-31.667	262.645073	-31.633306	264.364444	-8.35361	356.33349006	0.70266893	94.2779	54916.2757060185	2009-03-26 06:37:01	54917.0786921296	2009-03-27 01:53:19	503023010	31.1527	40	31.1527	31.1527	0	31.1527	2	2	0	2	1	0	0	28.2346	28.2346	69.3699	0	PROCESSED	57545.9012615741	2016-06-06 21:37:49	55330	2010-05-14 00:00:00	54930.234849537	2009-04-09 05:38:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030023	NANTEN telescope discovered huge molecular loops in the galactic center region. The model that the huge loops is due to magnetic buoyancy caused by the Parkey instability is proposed. The loops size is 12 order of magnitude larger than the solar loops, but the physics would be common. X-ray emission from shock heated and/or accelerated particles would be expected at the foot point of the loops. We propose an X-ray observation at the foot point of the molecular loop with Suzaku and investigate the magnetic activity in the galactic scale.	GALACTIC DIFFUSE EMISSION	5	C	SHIGEO YAMAUCHI		JAP	3	AO3	SUZAKU OBSERVATION OF MOLECULAR LOOPS IN THE GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503023010/	Quick Look
337	CYGNUS LOOP (P11)	312.4425	31.5127	311.927752	31.32576	327.295676	46.874223	74.4826992	-7.83027866	49.9999	54595.9014814815	2008-05-09 21:38:08	54596.7391087963	2008-05-10 17:44:19	503055010	31.8947	25	31.9027	31.8947	0	31.9107	2	2	0	2	1	0	0	25.0738	25.0738	72.3599	0	PROCESSED	57542.4981712963	2016-06-03 11:57:22	54972	2009-05-21 00:00:00	54606.1436342593	2008-05-20 03:26:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503055010/	Quick Look
338	ASO0449	299.6429	28.7759	299.134977	28.639283	310.497072	48.135601	65.87759933	-0.32938525	56.1427	54974.6386921296	2009-05-23 15:19:43	54975.5786342593	2009-05-24 13:53:14	504044010	38.7337	20	38.7337	38.7417	0	38.7417	1	1	0	1	1	0	0	35.22	35.22	81.1999	2	PROCESSED	57546.6654050926	2016-06-07 15:58:11	55356	2010-06-09 00:00:00	54987.4424652778	2009-06-05 10:37:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 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 DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504044010/	Quick Look
339	ASO0447	298.557	28.6365	298.049709	28.504502	309.068665	48.278589	65.2636943	0.41202338	90.516	54928.7514699074	2009-04-07 18:02:07	54929.253587963	2009-04-08 06:05:10	504046010	20.5457	20	20.5457	20.5457	0	20.5457	2	2	0	2	1	0	0	16.9071	16.9071	43.3779	1	PROCESSED	57546.0447106482	2016-06-07 01:04:23	55324	2010-05-08 00:00:00	54949.4485300926	2009-04-28 10:45:53	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 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 DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504046010/	Quick Look
340	CYGNUS LOOP (P24)	312.134	32.2905	311.623759	32.104666	327.393235	47.692301	74.93132331	-7.14055521	61.3941	54621.1479513889	2008-06-04 03:33:03	54621.6271875	2008-06-04 15:03:09	503060010	18.5046	15	18.5046	18.5046	0	18.5046	2	2	0	2	1	0	0	14.999	14.999	41.3979	1	PROCESSED	57542.7234027778	2016-06-03 17:21:42	55003	2009-06-21 00:00:00	54637.4594675926	2008-06-20 11:01:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503060010/	Quick Look
341	(L,B)=(0.107,-1.425)	267.8602	-29.5833	267.06157	-29.570962	268.118883	-6.156195	0.10035042	-1.42140103	68.0986	55261.1636226852	2010-03-06 03:55:37	55263.893275463	2010-03-08 21:26:19	504050010	100.3991	100	100.4311	100.3991	0	100.4231	2	2	0	2	1	0	0	80.536	80.536	235.8218	1	PROCESSED	57550.8323726852	2016-06-11 19:58:37	55645	2011-03-25 00:00:00	55278.4832523148	2010-03-23 11:35:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040109	In order to resolve origin of the Galactic bulge/ridge emission, we propose to observe the blank field 1.5 deg from the Galactic center where Chandra recently performed the deepest exposure (900 ksec) aiming to resolve the Galactic "diffuse" emission into point sources. Goals of the present observation are the following: (1) Resolve the three iron emission lines (6.41 keV, 6.67 keV and 6.97 keV) with Suzaku, and compare with the point source population determined by Chandra to clarify what kinds of sources are responsible for which emission line. (2) Study Galactic latitudinal variation of the three emission lines comparing with the existent Suzaku observation at (l,b)=(0.0, -2.0). (3) Constrain the hard-tail emission above 10 keV, and study its Galactic latitudinal variation.	GALACTIC DIFFUSE EMISSION	5	B	KEN EBISAWA		JAP	4	AO4	RESOLVING ORIGIN OF THE IRON EMISSION LINES FROM THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504050010/	Quick Look
342	GC(0,-1.6)	268.0544	-29.7594	267.254612	-29.748002	268.29113	-6.329868	0.03481768	-1.65633011	65.7488	54899.6540509259	2009-03-09 15:41:50	54900.8168865741	2009-03-10 19:36:19	503081010	59.2233	50	59.2233	59.2233	0	59.2233	2	2	0	2	1	0	0	57.6018	57.6018	100.4538	1	PROCESSED	57545.7843402778	2016-06-06 18:49:27	55330	2010-05-14 00:00:00	54916.3813194444	2009-03-26 09:09:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030131	We propose a 50 ksec observation of very enigmatic diffuse structure at 1.6 degree south from the Galactic center. We first discovered this structure with ROSAT. Then with ASCA, we found that the spectrum exhibits thin thermal emission accompanied with a hard tail which may be nonthermal radiation from high energy electrons. These results imply presence of a strong shock in this region, possibly due to a jet from Sgr A*. The diffuse emission may be a fossil of the past activities. With the observation of Suzaku, we obtain the richest statistics ever achieved. Then we will reveal the shock front from the image, and verify the past activities of the massive blackhole.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI MURAKAMI		JAP	3	AO3	NEW EVIDENCE OF THE PAST ACTIVITY IN THE GALACTIC CENTER REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503081010/	Quick Look
343	TYCHO SNR	6.3115	64.1447	5.611508	63.867881	42.842768	53.765034	120.08050675	1.41805528	43.1557	54689.3425578704	2008-08-11 08:13:17	54690.918275463	2008-08-12 22:02:19	503085020	102.8556	100	102.8556	102.8556	0	102.8556	2	2	0	2	1	0	0	91.9078	91.9078	136.1039	1	PROCESSED	57543.2895717593	2016-06-04 06:56:59	54557	2008-04-01 00:00:00	54706.7896412037	2008-08-28 18:57:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031003	Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		USA	3	AO3	SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503085020/	Quick Look
344	GCL1	265.1726	-28.5274	264.381201	-28.50205	265.733071	-5.157711	359.7799359	1.13423351	69.7267	54900.8188425926	2009-03-10 19:39:08	54901.4557175926	2009-03-11 10:56:14	503099010	29.706	25	29.7241	29.722	0	29.706	2	2	0	2	1	0	0	30.5649	30.5649	55.02	1	PROCESSED	57545.7841782407	2016-06-06 18:49:13	55329	2010-05-13 00:00:00	54916.3706828704	2009-03-26 08:53:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031234	We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity.	GALACTIC DIFFUSE EMISSION	5	B	FARHAD YUSEF-ZADEH		USA	3	AO3	A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503099010/	Quick Look
345	HESSJ1616_PSRJ1617	244.3756	-50.9175	243.427641	-50.794985	251.811911	-29.080089	332.50297445	-0.27465368	270.0711	55059.1110763889	2009-08-16 02:39:57	55060.8328009259	2009-08-17 19:59:14	504056010	65.8331	50	65.8891	65.8331	0	65.8971	2	2	0	2	1	0	0	41.7504	41.7504	148.7258	0	PROCESSED	57548.1892708333	2016-06-09 04:32:33	55437	2010-08-29 00:00:00	55071.2513425926	2009-08-28 06:01:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040115	HESSJ1616-508 is one of the most energetic unidentified TeV object. Previously, we showed that there is no clear X-ray counterpart to this object with a Suzaku observation, and hence we argued that the object is a real dark particle accelerator. However, there is a young energetic pulsar PSRJ1617-5055 10 arcmin away from HESSJ1616, and another possibility has been proposed that HESSJ1616 is an offset pulsar wind nebula (PWN) driven by the pulsar. If this possibility is correct, a powerful X-ray PWN should be observed as HESSJ1825-137, but such PWN has not been reported. The lack of the detection may be due to small sensitivity of Chandra and XMM-Newton for a diffuse hard X-ray emission. We propose to observe PSRJ1617 to see if there is an extended PWN around this pulsar.	GALACTIC DIFFUSE EMISSION	5	A	HIRONORI MATSUMOTO		JAP	4	AO4	IS THE MOST ENERGETIC UNIDENTIFIED TEV OBJECT HESSJ1616-508 A PULSAR WIND NEBULA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504056010/	Quick Look
346	SLX 1737-282	265.2352	-28.3094	264.445148	-28.284356	265.781005	-4.938001	359.99405573	1.20298654	69.9745	54901.4562384259	2009-03-11 10:56:59	54901.8035648148	2009-03-11 19:17:08	503103010	18.316	10	18.3324	18.332	0	18.316	2	2	0	2	1	0	0	16.3659	16.3659	30.0019	0	PROCESSED	57545.7980208333	2016-06-06 19:09:09	55329	2010-05-13 00:00:00	54916.9907638889	2009-03-26 23:46:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031234	We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity.	GALACTIC DIFFUSE EMISSION	5	C	FARHAD YUSEF-ZADEH		USA	3	AO3	A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503103010/	Quick Look
347	HESS J1745-303C	266.3881	-30.6242	265.582985	-30.604704	266.857963	-7.222423	358.55151469	-0.86700864	101.7444	55252.1897800926	2010-02-25 04:33:17	55253.3842476852	2010-02-26 09:13:19	504003010	50.9065	50	50.9145	50.9145	0	50.9065	2	2	0	2	1	0	0	41.2708	41.2708	103.1878	3	PROCESSED	57550.7231365741	2016-06-11 17:21:19	55632	2011-03-12 00:00:00	55264.3901157407	2010-03-09 09:21:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040001	The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	4	AO4	DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504003010/	Quick Look
348	TYCHO SNR	6.3244	64.1507	5.624265	63.873888	42.856632	53.765731	120.08671326	1.42345384	81.1044	53913.439224537	2006-06-27 10:32:29	53915.6530555556	2006-06-29 15:40:24	500024010	101.1274	100	101.1434	101.1274	101.1434	101.1434	2	2	2	2	1	0	0	94.5123	94.5123	191.2068	3	PROCESSED	57534.8252199074	2016-05-26 19:48:19	54289	2007-07-08 00:00:00	54052.7199884259	2006-11-13 17:16:47	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001099	We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		JAP	0	SWG	SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500024010/	Quick Look
349	NEP #3	270.0483	66.5696	270.04982	66.569341	34.92017	89.983512	96.39421541	29.79223028	188.0738	55180.9320949074	2009-12-15 22:22:13	55182.0557638889	2009-12-17 01:20:18	504074010	50.1769	50	50.1769	50.1769	0	50.1769	2	2	0	2	1	0	0	33.3374	33.3374	97.0499	1	PROCESSED	57549.895162037	2016-06-10 21:29:02	54922	2009-04-01 00:00:00	55200.4707291667	2010-01-04 11:17:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041101	We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe.	GALACTIC DIFFUSE EMISSION	5	A	STEVEN SNOWDEN		USA	4	AO4	OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504074010/	Quick Look
350	HESS J1809-193E	272.0013	-19.5033	271.261943	-19.51123	271.881238	3.92439	10.71539243	0.332309	270.1011	55085.7498148148	2009-09-11 17:59:44	55087.1564351852	2009-09-13 03:45:16	504079010	51.0289	50	51.0289	51.0289	0	51.0289	2	2	0	2	1	0	0	41.8753	41.8753	121.5198	2	PROCESSED	57548.5914699074	2016-06-09 14:11:43	55465	2010-09-26 00:00:00	55098.3372337963	2009-09-24 08:05:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041303	We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background.	GALACTIC DIFFUSE EMISSION	5	A	OLEG KARGALTSEV		USA	4	AO4	CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504079010/	Quick Look
351	G156.2+5.7 (NW2)	74.4322	52.0607	73.448956	51.983713	79.105505	29.208158	155.84514532	5.68920631	266.0115	55258.7553587963	2010-03-03 18:07:43	55259.9821643518	2010-03-04 23:34:19	504081010	52.8646	50	52.8678	52.8678	0	52.8646	2	2	0	2	1	0	0	49.3866	49.3866	105.991	1	PROCESSED	57550.7899189815	2016-06-11 18:57:29	55689	2011-05-08 00:00:00	55322.3173842593	2010-05-06 07:37:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041311	The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks.	GALACTIC DIFFUSE EMISSION	5	C	SATORU KATSUDA		USA	4	AO4	REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504081010/	Quick Look
352	330.2+1.0	240.2338	-51.588	239.290439	-51.447752	249.06097	-30.286548	330.14009051	0.98414205	285.0002	55078.1480671296	2009-09-04 03:33:13	55080.8126736111	2009-09-06 19:30:15	504083010	127.7746	150	127.7826	127.7746	0	127.7746	2	2	0	2	1	0	0	112.8484	112.8484	230.1578	1	PROCESSED	57548.4938657407	2016-06-09 11:51:10	55455	2010-09-16 00:00:00	55089.3295949074	2009-09-15 07:54:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041312	Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity.	GALACTIC DIFFUSE EMISSION	5	B	GLENN ALLEN		USA	4	AO4	MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504083010/	Quick Look
353	RXJ1713-3946	258.1633	-39.7281	257.296672	-39.668915	260.511599	-16.675371	347.25895477	-0.31287235	268.0002	53989.5311574074	2006-09-11 12:44:52	53989.9216898148	2006-09-11 22:07:14	501064010	21.322	20	21.322	21.322	21.322	21.322	2	2	2	2	1	0	0	23.0306	23.0306	33.7279	0	PROCESSED	57535.5353356482	2016-05-27 12:50:53	54526	2008-03-01 00:00:00	54020.8109027778	2006-10-12 19:27:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501064010/	Quick Look
354	SGR_B2	266.8776	-28.4437	266.086356	-28.426612	267.234654	-5.032575	0.63615824	-0.0985299	266.3663	55095.6093518518	2009-09-21 14:37:28	55096.0418287037	2009-09-22 01:00:14	504004010	10.0572	200	10.0572	10.0572	0	10.0572	2	2	0	2	1	0	0	9.4328	9.4328	37.3409	0	PROCESSED	57548.6152314815	2016-06-09 14:45:56	55476	2010-10-07 00:00:00	55110.2035763889	2009-10-06 04:53:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040002	The Galactic center diffuse X-ray emission (GCDX) consists of the hot plasma, neutral iron line, and hard tail. While we have demonstrated the hot plasma truly extending, origins of the others are still under discussion. We found time variability of the neutral Fe line intensity and marginally detected neutral lines of S, Ar, and Ca from Sagittarius B2. Our purpose is to clearly detect the neutral lines of S, Ar, Ca, and time variability of the hard tail of the GCDX up to 40 keV. This observation will resolve the remaining mysteries of the GCDX.	GALACTIC DIFFUSE EMISSION	5	A	MASAYOSHI NOBUKAWA		JAP	4	AO4	SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION-	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504004010/	Quick Look
355	RIM4	311.4678	31.0131	310.952491	30.829697	325.890411	46.737501	73.56601773	-7.48621797	246.0303	55155.1210763889	2009-11-20 02:54:21	55155.3579166667	2009-11-20 08:35:24	504008010	12.1025	10	12.1025	12.1185	0	12.1105	1	1	0	1	1	0	0	8.666	8.666	20.4559	0	PROCESSED	57549.475462963	2016-06-10 11:24:40	55534	2010-12-04 00:00:00	55166.425787037	2009-12-01 10:13:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504008010/	Quick Look
356	NEP	272.8227	66.0165	272.806643	66.002812	335.593486	88.746745	95.79277142	28.663354	126.3033	53776.2556944445	2006-02-10 06:08:12	53778.0836111111	2006-02-12 02:00:24	500026010	88.5082	80	88.5322	88.5082	88.5242	88.5322	2	2	2	2	1	0	0	83.6728	83.6728	157.902	0	PROCESSED	57532.9856481482	2016-05-24 23:39:20	54247	2007-05-27 00:00:00	54041.1403703704	2006-11-02 03:22:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000042	We propose a second Suzaku observation of the NEP region in order to constrain the long-term and short-term valiability of OVII and OIVVV emission line intensities.Short-term variability detected in the first Suzaku observation implies existence of a charge-exchange component in oVIII linem suggesting solar wind and geo corona interaction. First purpose is to confirm this with the second observtaion.Secondly, to search a long-term variability. If it is observed, it will place a further constraints on the solar wind and interplanetary medium near the Earth.	GALACTIC DIFFUSE EMISSION	5	A	SWG		JAP	0	SWG	NEP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500026010/	Quick Look
357	BLOWOUT6	311.7638	30.9468	311.247593	30.762319	326.194522	46.578638	73.67127235	-7.72686898	241.7587	55165.8330787037	2009-11-30 19:59:38	55166.2883449074	2009-12-01 06:55:13	504016010	21	19	21.008	21.016	0	21	1	1	0	1	1	0	0	17.7129	17.7129	39.3279	0	PROCESSED	57549.644849537	2016-06-10 15:28:35	55547	2010-12-17 00:00:00	55181.2630324074	2009-12-16 06:18:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504016010/	Quick Look
358	GALACTIC_BULGE2	267.5552	-29.599	266.756514	-29.585181	267.852413	-6.176134	359.95115697	-1.20153587	277.9812	55113.1708217593	2009-10-09 04:05:59	55114.5903472222	2009-10-10 14:10:06	504089010	55.2601	50	55.2671	55.2601	0	55.2736	2	2	0	2	1	0	0	40.226	40.226	122.6338	1	PROCESSED	57548.8316666667	2016-06-09 19:57:36	54922	2009-04-01 00:00:00	55131.3309953704	2009-10-27 07:56:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504089010/	Quick Look
359	HESS J1427-608	216.9609	-60.8505	216.024633	-60.626609	237.709544	-43.214788	314.40487303	-0.14444396	90.5578	55209.5761458333	2010-01-13 13:49:39	55212.1891666667	2010-01-16 04:32:24	504034010	104.1379	100	104.1379	104.1379	0	104.1379	2	2	0	2	1	0	0	71.2611	71.2611	225.7378	1	PROCESSED	57550.2389930556	2016-06-11 05:44:09	55594	2011-02-02 00:00:00	55225.4958449074	2010-01-29 11:54:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040066	Pulsar wind nebula (PWN) has began to be recognized as the best candidate of a large fraction of the HESS-unidentified (unID) sources. It could be true for some sources like HESS J1825-137, while other PWN candidates are sometimes listed simply because they satisfy one or two of the necessary conditions (e.g., there is an energetic pulsar nearby). We then propose a Suzaku observation of HESS J1427-608, which is the most ``unlike'' HESS-unID source to be a PWN. The advantage that we can safely exclude a PWN for its candidate allows us to identify the emission mechanism/origin of HESS J1427-608 more unambiguously compared to other unID sources. We request a 150 ks exposure to constrain the ratio between X-ray and TeV fluxes, which is a good measure of the emission mechanism of TeV sources.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	4	AO4	A SUZAKU OBSERVATION OF HESS J1427-608	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504034010/	Quick Look
360	ASO0402	273.3436	-12.7608	272.639832	-12.775336	273.308329	10.641449	17.24676471	2.45193699	68.9842	55277.3929513889	2010-03-22 09:25:51	55277.9793287037	2010-03-22 23:30:14	504042010	25.7125	20	25.7125	25.7125	0	25.7125	1	1	0	1	1	0	0	16.0152	16.0152	50.6559	1	PROCESSED	57550.9498958333	2016-06-11 22:47:51	55784	2011-08-11 00:00:00	55417.0893865741	2010-08-09 02:08:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 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 DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504042010/	Quick Look
361	73P/SW3	18.0599	-9.2267	17.433228	-9.491881	13.014248	-15.596574	139.25333623	-71.43625621	59.4006	53894.0025	2006-06-08 00:03:36	53894.0689699074	2006-06-08 01:39:19	500014060	3.235	35	3.235	3.235	3.235	3.235	1	1	1	1	1	0	0	2.49	2.49	5.7359	0	PROCESSED	57534.5883796296	2016-05-26 14:07:16	54267	2007-06-16 00:00:00	54052.5346759259	2006-11-13 12:49:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014060/	Quick Look
362	73P/SW3	18.338	-9.3332	17.711705	-9.597966	13.233056	-15.802283	140.17356876	-71.46762322	59.3974	53894.4024768518	2006-06-08 09:39:34	53894.4682986111	2006-06-08 11:14:21	500014120	1.5551	35	1.5551	1.5551	1.5551	1.5551	1	1	1	1	1	0	0	1.566	1.566	5.682	0	PROCESSED	57534.5988773148	2016-05-26 14:22:23	54267	2007-06-16 00:00:00	54052.5441782407	2006-11-13 13:03:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014120/	Quick Look
363	SN1006 SE	225.8656	-42.0517	225.046486	-41.856364	235.600187	-23.734349	327.61589547	14.40537	115.0022	53765.3759259259	2006-01-30 09:01:20	53766.487662037	2006-01-31 11:42:14	500016010	51.6076	50	51.6132	51.6212	51.6212	51.6076	2	2	2	2	1	0	0	55.6704	55.6704	96.0399	2	PROCESSED	57532.8333564815	2016-05-24 20:00:02	54247	2007-05-27 00:00:00	54040.6484259259	2006-11-01 15:33:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001062	We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		JAP	0	SWG	THE EJECTA IN SN1006	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500016010/	Quick Look
364	SGR C	266.1523	-29.4673	265.354719	-29.446679	266.622211	-6.071258	359.43182832	-0.08906822	82.0001	53786.5315393518	2006-02-20 12:45:25	53789.4515509259	2006-02-23 10:50:14	500018010	106.9219	100	106.9219	106.9219	106.9219	106.9219	2	2	2	2	1	0	0	46.6069	46.6069	252.2778	2	PROCESSED	57533.0732175926	2016-05-25 01:45:26	54247	2007-05-27 00:00:00	54041.6109375	2006-11-02 14:39:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001079	We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI MURAKAMI		JAP	0	SWG	FOSSILS OF THE GALACTIC CENTER ACTIVITY	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500018010/	Quick Look
365	VICINITY OF NGC 4051	180.4686	44.1146	179.828661	44.392934	159.283243	39.862026	150.13143213	70.30340869	109.3717	55184.3459606482	2009-12-19 08:18:11	55186.5140509259	2009-12-21 12:20:14	504062010	89.6305	80	89.6385	89.6465	0	89.6305	3	2	0	2	1	0	0	37.0758	37.0758	187.2819	2	PROCESSED	57549.977337963	2016-06-10 23:27:22	55581	2011-01-20 00:00:00	55209.4570833333	2010-01-13 10:58:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040120	The highly ionized absorption lines of OVII and OVII at z = 0 have been unambiguously detected toward the bright AGN NGC 4051 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII and OVIII emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas.	GALACTIC DIFFUSE EMISSION	5	C	TOSHISHIGE HAGIHARA		JAP	4	AO4	STUDY OF WARM-HOT GAS TOWARD NGC 4051	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504062010/	Quick Look
366	W51NW	290.6858	14.2133	290.110894	14.116258	294.988251	35.876885	49.11550833	-0.31636783	105.4558	55283.4893634259	2010-03-28 11:44:41	55284.555	2010-03-29 13:19:12	504066010	44.1125	40	44.1205	44.1205	0	44.1125	1	1	0	1	1	0	0	8.8961	8.8961	92.0639	0	PROCESSED	57551.0258217593	2016-06-12 00:37:11	55671	2011-04-20 00:00:00	55302.5003240741	2010-04-16 12:00:28	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040129	We propose to observe the supernova remnant (SNR) W51C with Suzaku XIS. The thermal energy of plasma in W51C, ~3x10^51ergs, is much larger than typical kinetic energy of supernova and can give a large amount of energy to cosmic-ray acceleration. The SNR interactes with the giant molecler cloud and is expected to emit gamma-rays from cosmic-ray interaction. We search for non-thermal X-ray diffuse emission from electron bremsstrahlung or synchrotron emission of secondary electrons produced by decaying charged pions created by p-p interaction.	GALACTIC DIFFUSE EMISSION	5	C	HIDEAKI KATAGIRI		JAP	4	AO4	ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504066010/	Quick Look
367	SEP #3	89.9578	-66.5683	89.959755	-66.568521	317.285609	-89.984917	276.39273536	-29.82821774	172.4885	55179.5059259259	2009-12-14 12:08:32	55180.9169444444	2009-12-15 22:00:24	504073010	44.408	50	44.408	44.416	0	44.416	2	2	0	2	1	0	0	23.8784	23.8784	121.9018	1	PROCESSED	57549.8504282407	2016-06-10 20:24:37	54922	2009-04-01 00:00:00	55200.462337963	2010-01-04 11:05:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041101	We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe.	GALACTIC DIFFUSE EMISSION	5	A	STEVEN SNOWDEN		USA	4	AO4	OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504073010/	Quick Look
368	CYGNUS_LOOP_P2	313.2729	31.7708	312.75774	31.580892	328.394465	46.831624	75.13379207	-8.21853117	240.0005	54418.0909722222	2007-11-14 02:11:00	54418.4168865741	2007-11-14 10:00:19	501013010	16.3799	10	16.3879	16.3879	0	16.3799	1	1	0	1	1	0	0	10.9786	10.9786	28.1519	0	PROCESSED	57540.5114351852	2016-06-01 12:16:28	54798	2008-11-28 00:00:00	54430.1915972222	2007-11-26 04:35:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501013010/	Quick Look
369	G156.2+5.7 (E2)	75.2673	51.6789	74.287315	51.605827	79.638917	28.767744	156.46612231	5.86221802	271.6298	55248.7736574074	2010-02-21 18:34:04	55250.0369675926	2010-02-23 00:53:14	504082010	50.3308	50	50.3468	50.3308	0	50.3468	3	2	0	2	1	0	0	46.1424	46.1424	109.1379	0	PROCESSED	57550.6943865741	2016-06-11 16:39:55	55632	2011-03-12 00:00:00	55266.2981597222	2010-03-11 07:09:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041311	The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks.	GALACTIC DIFFUSE EMISSION	5	C	SATORU KATSUDA		USA	4	AO4	REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504082010/	Quick Look
370	CYGNUS_LOOP_P14	313.2365	30.8681	312.717032	30.678328	327.835222	46.014729	74.40554659	-8.76356285	62.362	53867.6311111111	2006-05-12 15:08:48	53868.0050462963	2006-05-13 00:07:16	501031010	18.5809	18	18.5809	18.5809	18.5809	18.5809	2	2	2	2	1	0	0	12.7378	12.7378	32.2979	0	PROCESSED	57534.275775463	2016-05-26 06:37:07	54394	2007-10-21 00:00:00	53914.3142476852	2006-06-28 07:32:31	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501031010/	Quick Look
371	KEPLER_BG_GE	263.5353	-20.2634	262.792573	-20.230259	263.918925	3.041235	5.99742641	6.79731937	272.7609	55087.1593171296	2009-09-13 03:49:25	55088.3606365741	2009-09-14 08:39:19	504101010	46.9895	60	46.9895	46.9895	0	46.9895	2	2	0	2	1	0	0	40.8993	40.8993	103.786	0	PROCESSED	57548.5758564815	2016-06-09 13:49:14	54922	2009-04-01 00:00:00	55099.2516782407	2009-09-25 06:02:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	4	AO4	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504101010/	Quick Look
372	IC443 NORTHWEST	93.9975	22.7552	93.240341	22.772771	93.68801	-0.634546	188.75644855	2.86235674	91.4819	55456.3191435185	2010-09-17 07:39:34	55458.2829050926	2010-09-19 06:47:23	505001010	83.1917	80	83.1917	83.1917	0	83.1917	2	2	0	2	1	0	0	69.6786	69.6786	169.6457	2	PROCESSED	57553.4791087963	2016-06-14 11:29:55	55836	2011-10-02 00:00:00	55469.4041087963	2010-09-30 09:41:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050001	Suzaku discovered the radiative recombination continua (RRC) of Si and S from the supernova remnant IC443. This new phenomenon (the RRC) would be due to either pre-ionization by X-ray flash of gamma-ray burst, or adiabatic cooling in a rarefied ambient medium, or yet-unknown process. In any case, the RRC have essential and new clues for the mechanisms, evolution and/or even the cosmic-ray acceleration of IC443. Spectra of the rim regions provide key information for the RRC origin. We thus propose the East and West periphery of IC443 for total 200 ksec.	GALACTIC DIFFUSE EMISSION	5	C	MIDORI OZAWA		JAP	5	AO5	EXPLORING THE ORIGIN OF THE RADIATIVE RECOMBINATION CONTINUUM OF IC443	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505001010/	Quick Look
373	CYGNUS_LOOP_P18	312.0547	29.7111	311.531939	29.525574	325.8489	45.340722	72.84665082	-8.68804998	237.4994	54087.0528819444	2006-12-18 01:16:09	54087.3405208333	2006-12-18 08:10:21	501035010	12.011	13	12.915	12.011	0	12.907	2	2	0	2	1	0	0	11.4394	11.4394	24.8359	3	PROCESSED	57536.3543981482	2016-05-28 08:30:20	54750	2008-10-11 00:00:00	54096.4390972222	2006-12-27 10:32:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501035010/	Quick Look
374	CYGNUS LOOP 7	313.929	31.0152	313.408854	30.822982	328.70395	45.915608	74.90122685	-9.13052292	81.814	55306.459212963	2010-04-20 11:01:16	55306.7974189815	2010-04-20 19:08:17	505015010	13.5918	12	13.5918	13.5998	0	13.5998	2	2	0	2	1	0	0	12.682	12.682	29.1959	0	PROCESSED	57551.269212963	2016-06-12 06:27:40	55287	2010-04-01 00:00:00	55393.2216203704	2010-07-16 05:19:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505015010/	Quick Look
375	CYGNUS LOOP 14	313.0411	29.9656	312.517703	29.77653	327.111212	45.248773	73.58742167	-9.19932348	67.2195	55334.4727893518	2010-05-18 11:20:49	55335.1146759259	2010-05-19 02:45:08	505022010	29.2512	29	29.2512	29.2512	0	29.2512	2	2	0	2	1	0	0	24.7832	24.7832	55.4519	0	PROCESSED	57551.5599305556	2016-06-12 13:26:18	55287	2010-04-01 00:00:00	55348.0488888889	2010-06-01 01:10:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505022010/	Quick Look
376	FVW319.8+0.3	225.913	-58.2332	224.953134	-58.037768	241.861071	-39.018553	319.61922846	0.28881447	278.3756	55413.1563888889	2010-08-05 03:45:12	55413.9307291667	2010-08-05 22:20:15	505029010	51.384	50	51.4	51.384	0	51.4	2	2	0	2	1	0	0	45.416	45.416	66.8939	2	PROCESSED	57552.8424421296	2016-06-13 20:13:07	55793	2011-08-20 00:00:00	55427.1529976852	2010-08-19 03:40:19	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050010	Forbidden-velocity wings (FVWs) are unknown HI clouds with high velocity dispersion. They could be old supernova remnants or star-forming bubbles, although the origin is unknown. Recently, TeV gamma-rays have been detected from one of the FVWs, FVW319.8+0.3, implying that it is a cosmic-ray accelerator. We will investigate this FVW with low-background observations of Suzaku, in order to search for thermal emission from the undiscovered supernova remnant. It is not only the first discovery of X-rays from FVWs, but also the first clue of the cosmic-ray acceleration in FVWs. Even if we could detect nothing, we can conclude that this source is a kind of gdark particle accelerators h with the proposed exposure.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	5	AO5	SEARCHING FOR COSMIC ACCELERATION IN A FORBIDDEN-VELOCITY WING: A NEW OLD SUPERNOVA REMNANT ?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505029010/	Quick Look
377	HESS J1825-137 BG	276.9022	-13.2649	276.196149	-13.29666	276.811822	10.012623	18.4366217	-0.84356166	269.33	54027.1689351852	2006-10-19 04:03:16	54028.5072337963	2006-10-20 12:10:25	501045010	52.1444	50	52.1524	52.1444	52.1524	52.1444	2	2	2	2	1	0	0	42.1974	42.1974	115.6079	2	PROCESSED	57535.8869907407	2016-05-27 21:17:16	54526	2008-03-01 00:00:00	54055.6591550926	2006-11-16 15:49:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010073	We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	1	AO1	SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501045010/	Quick Look
378	L139_B-32	28.093	28.6837	27.38183	28.437322	36.368533	16.024453	138.75887563	-32.3084393	253.9538	55569.4091319444	2011-01-08 09:49:09	55571.3188541667	2011-01-10 07:39:09	505044010	84.0041	80	84.0041	84.0041	0	84.0041	2	2	0	2	1	0	0	79.0377	79.0377	164.9839	0	PROCESSED	57600.6057175926	2016-07-31 14:32:14	55962	2012-02-05 00:00:00	55595.2037615741	2011-02-03 04:53:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050064	Suzaku measurements of the large scale variation of the Halo emission surrounding our Galaxy are proposed. To minimize the local emission and absorption structure, we selected three pointings toward the anti-center region (l=140) of the Galactic latitude between-20 and -40.	GALACTIC DIFFUSE EMISSION	5	C	NORIKO YAMASAKI		JAP	5	AO5	STRUCTURE OF THE GALACTIC HALO EMISSION TOWARD THE ANTI-CENTER REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505044010/	Quick Look
379	PUP A : S	125.6829	-43.1445	125.254263	-42.982932	147.449231	-59.669734	260.57740663	-3.43620983	277.8865	53843.8334606482	2006-04-18 20:00:11	53844.4397569444	2006-04-19 10:33:15	501090010	31.1445	30	31.1605	31.1525	31.1445	31.1685	2	2	2	2	1	0	0	26.5856	26.5856	52.3719	1	PROCESSED	57533.5191550926	2016-05-25 12:27:35	54401	2007-10-28 00:00:00	53907.0902199074	2006-06-21 02:09:55	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501090010/	Quick Look
380	DEM L238	83.8177	-70.5927	83.963728	-70.62236	296.31824	-85.384034	281.24911245	-31.77318091	307.401	55308.023125	2010-04-22 00:33:18	55312.9730902778	2010-04-26 23:21:15	505063010	199.7795	200	199.7795	199.7795	0	199.7795	2	2	0	2	1	0	0	167.8355	167.8355	427.6297	5	PROCESSED	57551.4910069444	2016-06-12 11:47:03	55287	2010-04-01 00:00:00	55326.6889699074	2010-05-10 16:32:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051102	Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors.	GALACTIC DIFFUSE EMISSION	5	A	KAZIMIERZ BORKOWSKI		USA	5	AO5	TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505063010/	Quick Look
381	THE KEPLER SNR	262.6737	-21.5073	261.92432	-21.469989	263.173689	1.760317	4.50532186	6.80830692	272.2663	55475.6914583333	2010-10-06 16:35:42	55478.2863194445	2010-10-09 06:52:18	505092020	111.1941	620	111.1941	111.2021	0	111.2021	2	2	0	2	1	0	0	99.8413	99.8413	224.1437	2	PROCESSED	57553.7268402778	2016-06-14 17:26:39	55287	2010-04-01 00:00:00	55488.3311689815	2010-10-19 07:56:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092020/	Quick Look
382	THE KEPLER SNR	262.671	-21.4826	261.921758	-21.445276	263.169925	1.784856	4.5248811	6.82377384	98.1034	55628.0376736111	2011-03-08 00:54:15	55632.2696643518	2011-03-12 06:28:19	505092050	84.5913	100	84.5913	85.6632	0	85.7192	4	3	0	3	1	0	0	122.4881	122.4881	365.616	3	PROCESSED	57601.284537037	2016-08-01 06:49:44	55287	2010-04-01 00:00:00	55648.4964699074	2011-03-28 11:54:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092050/	Quick Look
383	VELA FRAGMENT B	135.5139	-43.4767	135.058427	-43.278826	159.573758	-56.461444	265.2464603	1.98991007	89.0012	54044.6051388889	2006-11-05 14:31:24	54046.4341898148	2006-11-07 10:25:14	501085010	57.8804	60	57.8964	57.8804	57.8964	57.8964	2	2	2	2	1	0	0	56.9652	56.9652	158.0219	2	PROCESSED	57536.0751157407	2016-05-28 01:48:10	54695	2008-08-17 00:00:00	54091.4107175926	2006-12-22 09:51:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011245	Ejecta fragments from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM-Newton, show strongly enhanced but very different abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe another fragment, "B". The abundances and distribution will provide further evidence about the origin and evolution of these ejecta clumps, In combination with the existing observations of fragments A and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interaction with the remnant shell and the surrounding ISM.	GALACTIC DIFFUSE EMISSION	5	C	TERRANCE GAETZ		USA	1	AO1	SEARCHING FOR EJECTA IN VELA SNR FRAGMENT B	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501085010/	Quick Look
384	HB21 SOUTH	311.2512	50.6016	310.86516	50.418766	342.682858	64.005982	88.85305014	4.80482025	105.492	55660.3542361111	2011-04-09 08:30:06	55662.8155208333	2011-04-11 19:34:21	506005010	132.363	150	132.371	132.371	0	132.363	3	2	0	2	1	0	0	141.7887	141.7887	212.6359	1	PROCESSED	57601.4958564815	2016-08-01 11:54:02	56159	2012-08-20 00:00:00	55677.2811342593	2011-04-26 06:44:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060011	Over-ionization in SNRs is one of the biggest mystery Suzaku discovered. It affects a lot the study on chemical and thermal evolution of universe, but the origin is still unknown. HB21 is an old SNR with molecular cloud interaction and GeV gamma-rays, which remind us typical over-ionization SNRs. On the other hand, the interacting molecular cloud is much smaller or thinner than those interacting with over-ionization SNRs, and as a result, HB21 can be the key target to study the origin of over-ionization. Suzaku deep observation of HB21 south (interacting point) will determine the condition of plasma and judge whether it is in over-ionization or not, which will show us the origin of over-ionizing plasma.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	6	AO6	ORIGIN OF OVER-IONIZATION OF SNR PLASMAS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506005010/	Quick Look
385	CYGNUS LOOP BLOWOUT2	312.4423	29.4154	311.917417	29.228478	326.132278	44.939266	72.82314938	-9.13589092	78.1524	55687.8500578704	2011-05-06 20:24:05	55688.6488310185	2011-05-07 15:34:19	506012010	35.655	35	35.655	35.655	0	35.655	2	2	0	2	1	0	0	31.4815	31.4815	68.9821	0	PROCESSED	57601.9748263889	2016-08-01 23:23:45	56066	2012-05-19 00:00:00	55700.4593865741	2011-05-19 11:01:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060053	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	6	AO6	MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506012010/	Quick Look
386	VELA PULSAR/PWN 1	128.7701	-45.1981	128.348103	-45.024538	153.316878	-60.401286	263.5414959	-2.83747227	337.9628	53926.0492592593	2006-07-10 01:10:56	53927.7841782407	2006-07-11 18:49:13	501109010	60.2913	60	60.3446	60.2913	60.3313	60.3233	2	2	2	2	1	0	0	52.6899	52.6899	149.8659	1	PROCESSED	57534.9239699074	2016-05-26 22:10:31	54401	2007-10-28 00:00:00	53942.4588078704	2006-07-26 11:00:41	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014211	The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band.	GALACTIC DIFFUSE EMISSION	5	B	OLEG KARGALTSEV	KOJI MORI	USJ	1	AO1	THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501109010/	Quick Look
387	G272.2-3.2	136.7067	-52.1223	136.311595	-51.920282	170.81242	-63.078479	272.22054405	-3.18534238	101.7643	55877.9477777778	2011-11-12 22:44:48	55878.6272916667	2011-11-13 15:03:18	506060020	25.5265	20	25.5345	25.5345	0	25.5265	2	2	0	2	1	0	0	27.028	27.028	58.706	0	PROCESSED	57603.7829282407	2016-08-03 18:47:25	55652	2011-04-01 00:00:00	55895.0737962963	2011-11-30 01:46:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506060020/	Quick Look
388	CYGNUS LOOP BLOWOUT6	312.8964	28.9665	312.36858	28.777954	326.408889	44.373591	72.71699713	-9.72555156	78.1534	55691.9894791667	2011-05-10 23:44:51	55692.7710069445	2011-05-11 18:30:15	506016010	36.3744	35	36.3744	36.3744	0	36.3744	2	2	0	2	1	0	0	32.7568	32.7568	67.5039	0	PROCESSED	57602.0240277778	2016-08-02 00:34:36	56068	2012-05-21 00:00:00	55701.1981828704	2011-05-20 04:45:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060053	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	6	AO6	MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506016010/	Quick Look
389	GC23	266.578	-28.0524	265.789256	-28.033865	266.960919	-4.647397	0.83380185	0.3300796	262.2345	54386.7855208333	2007-10-13 18:51:09	54387.2294444444	2007-10-14 05:30:24	502011010	23.013	20	23.013	23.021	0	23.029	1	1	0	1	1	0	0	22.0712	22.0712	38.3199	2	PROCESSED	57540.2674305556	2016-06-01 06:25:06	54777	2008-11-07 00:00:00	54402.5316898148	2007-10-29 12:45:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502011010/	Quick Look
390	G23.5+0.1	278.489	-8.375	277.807565	-8.414468	278.678732	14.810155	23.49243074	0.03918587	261.7121	55489.5657291667	2010-10-20 13:34:39	55491.0730439815	2010-10-22 01:45:11	505026010	48.9761	50	48.9761	48.9761	0	48.9761	2	2	0	2	1	0	0	43.7884	43.7884	130.1919	0	PROCESSED	57553.8193981482	2016-06-14 19:39:56	55868	2011-11-03 00:00:00	55502.1887962963	2010-11-02 04:31:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050009	ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature.	GALACTIC DIFFUSE EMISSION	5	B	SHIGEO YAMAUCHI		JAP	5	AO5	SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505026010/	Quick Look
391	3C 59 VICINITY 2	31.4351	28.9234	30.715452	28.684984	39.296603	15.198203	141.95387958	-31.18906496	250.3	55952.5116435185	2012-01-26 12:16:46	55957.4238773148	2012-01-31 10:10:23	506025010	173.347	50	173.347	173.355	0	173.355	3	2	0	2	1	0	0	0.5479	0.5479	86.854	0	PROCESSED	57604.5146759259	2016-08-04 12:21:08	56526	2013-08-22 00:00:00	56167.6426388889	2012-08-28 15:25:24	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060067	We propose for an observation of the vicinities of 3C 59, in order to study the radial extent of the Galactic hot gas. We have conducted joint analysis of absorption and emission lines toward several targets until now and successfully constrained the temperature, line-of-sight length, and density of the hot gas of the directions. However, all the line-of-sight lengths of the hot gas for the past surveys stay within the Galactic disc with the radius of 10 kpc, therefore the radial extent of the gas is still unknown. Emission analysis of low-latitude and almost anti-center directed 3C 59 will constrain the extent, and the result will be unambiguous when emission and absorption lines are jointly analyzed.	GALACTIC DIFFUSE EMISSION	5	C	KAZUHIRO SAKAI		JAP	6	AO6	STUDY OF RADIAL DISTRIBUTION OF THE HOT INTERSTELLAR MEDIUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506025010/	Quick Look
392	VELA PWN E3	129.9962	-45.3672	129.571682	-45.189023	154.98711	-60.107857	264.19786494	-2.25193357	304.5033	55712.1335069444	2011-05-31 03:12:15	55712.4099305556	2011-05-31 09:50:18	506046010	14.1787	15	14.2027	14.1947	0	14.1787	2	2	0	2	1	0	0	12.6599	12.6599	23.8759	0	PROCESSED	57602.1638078704	2016-08-02 03:55:53	56093	2012-06-15 00:00:00	55725.9978240741	2011-06-13 23:56:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506046010/	Quick Look
393	RADIO_ARC_S_W	266.7778	-29.3674	265.980729	-29.349813	267.167421	-5.95796	359.8007683	-0.50226251	267.1999	56200.9358101852	2012-09-30 22:27:34	56202.0120601852	2012-10-02 00:17:22	507018010	51.0807	50	51.1047	51.0967	0	51.0807	3	2	0	2	1	0	0	49.115	49.115	92.9799	0	PROCESSED	57607.2580324074	2016-08-07 06:11:34	56592	2013-10-27 00:00:00	56226.6169675926	2012-10-26 14:48:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070016	The 6.4 keV emission associated with giant molecular clouds is the most prominent feature in the Galactic center region. So far, the origin has only been found and discussed in the X-ray reflection process. We propose deep observation at the Radio Arc to discover the 6.4 keV emission in the particle origin, which would open the window to study the nature of the Galactic cosmic ray.	GALACTIC DIFFUSE EMISSION	5	A	SYUKYO RYU		JAP	7	AO7	X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN --	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507018010/	Quick Look
394	G290.1-0.8	165.7447	-60.8884	165.228717	-60.618807	206.73964	-58.122992	290.11957377	-0.7436408	293.2659	55737.4551388889	2011-06-25 10:55:24	55740.5883333333	2011-06-28 14:07:12	506061010	110.5931	110	110.6091	110.5931	0	110.6011	2	2	0	2	1	0	0	99.3596	99.3596	270.6596	4	PROCESSED	57602.4993634259	2016-08-02 11:59:05	55652	2011-04-01 00:00:00	55775.3693287037	2011-08-02 08:51:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506061010/	Quick Look
395	FERMI_BUBBLE_N5	233.6225	8.0718	233.013762	8.238094	228.991173	26.481108	14.37791019	47.00724717	287.4992	56146.9871990741	2012-08-07 23:41:34	56147.4320949074	2012-08-08 10:22:13	507005010	21.7222	20	21.7222	21.7222	0	21.7222	2	2	0	2	1	0	0	19.5559	19.5559	38.4299	1	PROCESSED	57606.7961921296	2016-08-06 19:06:31	56535	2013-08-31 00:00:00	56169.0806944444	2012-08-30 01:56:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507005010/	Quick Look
396	FERMI_BUBBLE_S3	327.8758	-46.7423	327.0753	-46.977097	312.913491	-31.549758	351.52788223	-49.77060768	44.0052	56035.6752777778	2012-04-18 16:12:24	56036.133587963	2012-04-19 03:12:22	507011010	21.2336	20	21.2336	21.2336	0	21.2336	2	2	0	2	1	0	0	20.914	20.914	39.596	0	PROCESSED	57605.205787037	2016-08-05 04:56:20	56420	2013-05-08 00:00:00	56049.1986458333	2012-05-02 04:46:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507011010/	Quick Look
397	VELA JR P3	132.1192	-45.6039	131.689583	-45.417926	157.761308	-59.536255	265.30669647	-1.23070071	347.0044	54285.9040162037	2007-07-04 21:41:47	54286.1057175926	2007-07-05 02:32:14	502025010	10.298	10	10.298	10.298	0	10.298	1	1	0	1	1	0	0	6.726	6.726	17.4239	0	PROCESSED	57539.0955902778	2016-05-31 02:17:39	54696	2008-08-18 00:00:00	54328.4516782407	2007-08-16 10:50:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502025010/	Quick Look
398	IC 443	94.3024	22.7479	93.545319	22.766949	93.9693	-0.633748	188.89613959	3.10659531	258.9994	56388.2234837963	2013-04-06 05:21:49	56390.0835763889	2013-04-08 02:00:21	507015040	75.6427	300	75.6428	75.6427	0	75.6427	3	2	0	2	1	0	0	68.7284	68.7284	160.6759	1	PROCESSED	57611.01125	2016-08-11 00:16:12	56018	2012-04-01 00:00:00	56401.615775463	2013-04-19 14:46:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070015	The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	7	AO7	DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA --	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015040/	Quick Look
399	VELA JR P11	132.5986	-45.8258	132.169014	-45.638098	158.553222	-59.54754	265.69032827	-1.11165473	347.0024	54288.2314236111	2007-07-07 05:33:15	54288.6112731482	2007-07-07 14:40:14	502033010	11.2833	10	11.2833	11.2833	0	11.2833	2	2	0	2	1	0	0	12.2079	12.2079	32.7901	1	PROCESSED	57539.1206828704	2016-05-31 02:53:47	54696	2008-08-18 00:00:00	54328.4031944445	2007-08-16 09:40:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502033010/	Quick Look
400	VELA JR P22	132.4428	-46.6127	132.019624	-46.425546	159.213685	-60.269437	266.23093455	-1.69368029	346.9992	54652.0565625	2008-07-05 01:21:27	54652.3891087963	2008-07-05 09:20:19	503034010	15.2643	10	15.2643	15.2709	0	15.2709	2	2	0	2	1	0	0	14.9717	14.9717	28.728	0	PROCESSED	57542.966099537	2016-06-03 23:11:11	55036	2009-07-24 00:00:00	54670.1353125	2008-07-23 03:14:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503034010/	Quick Look
401	HESSJ1507-622_OFFSET	227.1815	-62.1646	226.158724	-61.973493	244.511164	-42.456937	318.2247639	-3.44071412	303.001	56183.9562268518	2012-09-13 22:56:58	56185.1042939815	2012-09-15 02:30:11	507026010	40.9122	40	40.9122	40.9418	0	40.9338	2	2	0	2	1	0	0	38.0336	38.0336	99.1798	1	PROCESSED	57607.0490162037	2016-08-07 01:10:35	56582	2013-10-17 00:00:00	56212.7288078704	2012-10-12 17:29:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070033	HESS J1507-622 is one of the unidentified TeV-gamma-ray sources discovered in the H.E.S.S. Galactic plane survey. The object is unique in the sense of the location, off the Galactic plane. There are no counterparts in radio, infrared, X-ray bands and thus the origin is still mystery, but the object represents several hints; X-ray source like pulsar wind nebula exists near the object, and the location is at the edge of the large molecular cloud near a radio supernova remnant. The main purpose of the Suzaku observation with the best use of high sensitive capability in diffuse X-rays and of a unique low galactic-absorption feature of the object is to determine the origin of TeV emission, such as old supernova remnant with molecular cloud, pulsar-wind driven radiations, or darkest accelerator.	GALACTIC DIFFUSE EMISSION	5	B	YUKIKATSU TERADA	HIRONORI MATSUMOTO	JAP	7	AO7	SUZAKU OBSERVATION OF HESS J1507-622; A UNIQUE TEV UNIDENTIFIED SOURCE OFF THE GALACTIC PLANE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507026010/	Quick Look
402	VELA JR P18	133.5064	-46.0415	133.075299	-45.850566	159.830487	-59.392209	266.25968404	-0.76370949	347.0006	54291.9244444444	2007-07-10 22:11:12	54292.1668634259	2007-07-11 04:00:17	502040010	15.0123	10	15.0123	15.0362	0	15.0203	2	2	0	2	1	0	0	12.8952	12.8952	20.9439	1	PROCESSED	57539.1482407407	2016-05-31 03:33:28	54696	2008-08-18 00:00:00	54328.4716666667	2007-08-16 11:19:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502040010/	Quick Look
403	LOW_LATITUDE_86-21	332.3169	30.2173	331.751825	29.971433	347.602182	38.425077	86.0039952	-20.78963339	82.7457	54229.0809259259	2007-05-09 01:56:32	54230.9966898148	2007-05-10 23:55:14	502047010	81.5486	80	81.5486	81.5486	0	81.5486	2	2	0	2	1	0	0	72.2931	72.2931	165.5099	2	PROCESSED	57538.6557986111	2016-05-30 15:44:21	54744	2008-10-05 00:00:00	54244.7948032407	2007-05-24 19:04:31	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020061	High galactic-latitude Suzaku observations of soft X-ray diffuse emission so far made show general tendency that the OVII emission line becomes stronger with decreasing abs(b). This suggests that the major part of the emission is originating from the halo of our galaxy. However, we cannot rule out the possibility that the data is contaminated by solar wind charge exchange emission from the entire heliosphere. In oder to confirm the abs(b) dependency and to constrain the spatial distribution of the halo emission, we propose to observe diffuse radiation at a low galactic latitude of abs(b) ~ 20 deg, where the galactic absorption still does not affect the line intensity significantly.	GALACTIC DIFFUSE EMISSION	5	B	TOMOTAKA YOSHINO		JAP	2	AO2	SOFT X-RAY DIFFUSE EMISSION AT A LOW GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502047010/	Quick Look
404	HESS J1457-593	224.4524	-59.4762	223.48511	-59.275761	241.535779	-40.451289	318.36335314	-0.44487967	305.8997	56185.1060185185	2012-09-15 02:32:40	56186.0216782407	2012-09-16 00:31:13	507027010	31.0479	30	31.0479	31.0479	0	31.0479	2	2	0	2	1	0	0	28.0994	28.0994	79.1059	1	PROCESSED	57607.0753819445	2016-08-07 01:48:33	56584	2013-10-19 00:00:00	56218.5178009259	2012-10-18 12:25:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070037	We propose an X-ray observation of the putative SNR-molecular cloud interaction HESS J1457-593 with the Suzaku XIS detector for 30 ks. The aim of the observation is to clarify whether the TeV gamma-ray emission is of a leptonic or hadronic origin by searching for an X-ray counterpart to a level down to $10^{-14}$~erg cm$^{-2}$ s$^{-1}$. A non-detection of an X-ray nebula would strongly disfavor a leptonic origin of the TeV emission and add to the already strong multi-wavelength data which all suggests a hadronic origin of the emission. Since the spectrum of this unique source extends above many tens of TeV this would mean that we see, for the first time, evidence for hadronic cosmic rays being accelerated up to PeV energies.	GALACTIC DIFFUSE EMISSION	5	B	HIROKAZU ODAKA		JAP	7	AO7	INVESTIGATING A PUTATIVE COSMIC-RAY PEVATRON WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507027010/	Quick Look
405	G298.6-0.0	183.3899	-62.6356	182.720759	-62.35751	219.490154	-53.509251	298.59488766	-0.08324812	319.8129	56150.8519097222	2012-08-11 20:26:45	56152.08625	2012-08-13 02:04:12	507037010	17.2388	50	17.2388	17.2388	0	17.2388	1	1	0	1	1	0	0	19.1746	19.1746	106.616	0	PROCESSED	57606.8422222222	2016-08-06 20:12:48	56721	2014-03-05 00:00:00	56291.7215162037	2012-12-30 17:18:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070047	A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem.	GALACTIC DIFFUSE EMISSION	5	B	AYA BAMBA		JAP	7	AO7	SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507037010/	Quick Look
406	CYG_COCOON	306.8026	40.9389	306.35518	40.773009	326.953221	57.33325	79.25133167	1.48664873	218.8996	56279.1800231482	2012-12-18 04:19:14	56280.1654976852	2012-12-19 03:58:19	507040010	51.0724	50	51.0724	51.0936	0	51.0804	2	2	0	2	1	0	0	42.7833	42.7833	85.1439	0	PROCESSED	57608.3232291667	2016-08-08 07:45:27	56683	2014-01-26 00:00:00	56316.5705324074	2013-01-24 13:41:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070060	The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object.	GALACTIC DIFFUSE EMISSION	5	C	TSUNEFUMI MIZUNO		JAP	7	AO7	SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507040010/	Quick Look
407	SNR HB3 SE-B	35.7593	62.192	34.815236	61.964819	57.837975	44.676486	133.39304715	1.19520932	247.4986	56323.4084259259	2013-01-31 09:48:08	56323.7710532407	2013-01-31 18:30:19	507057010	25.8366	20	25.8446	25.8366	0	25.8526	1	1	0	1	1	0	0	19.3092	19.3092	31.3279	1	PROCESSED	57608.6657638889	2016-08-08 15:58:42	56711	2014-02-23 00:00:00	56345.4750462963	2013-02-22 11:24:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071316	We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective.	GALACTIC DIFFUSE EMISSION	5	C	JUNICHIRO KATSUTA		USA	7	AO7	SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507057010/	Quick Look
408	SNR HB3 SE-C	36.0358	62.4578	35.086232	62.23139	58.169094	44.855041	133.42083063	1.4890972	247.4994	56323.7716666667	2013-01-31 18:31:12	56324.1585532407	2013-02-01 03:48:19	507058010	24.142	20	24.1616	24.142	0	24.1696	2	2	0	2	1	0	0	23.4547	23.4547	33.4239	0	PROCESSED	57608.6786342593	2016-08-08 16:17:14	56711	2014-02-23 00:00:00	56345.4779976852	2013-02-22 11:28:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071316	We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective.	GALACTIC DIFFUSE EMISSION	5	C	JUNICHIRO KATSUTA		USA	7	AO7	SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507058010/	Quick Look
409	COMET_8P_TUTTLE-P1-10	28.408	5.7525	27.75444	5.506869	28.446793	-5.529035	149.8061723	-53.84230192	248.5015	54471.1158333333	2008-01-06 02:46:48	54471.1820717593	2008-01-06 04:22:11	502062100	3.2196	3.2	3.2196	3.2196	0	3.2196	1	1	0	1	1	0	0	2.166	2.166	5.6799	0	PROCESSED	57541.2676967593	2016-06-02 06:25:29	54908	2009-03-18 00:00:00	54542.2429513889	2008-03-17 05:49:51	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062100/	Quick Look
410	G278.0+12.4	158.151	-43.7043	157.610146	-43.446336	182.388463	-47.807278	278.01040448	12.3478226	304.0284	56102.6152199074	2012-06-24 14:45:55	56102.9842476852	2012-06-24 23:37:19	507067010	18.996	17.5	19.004	18.996	0	19.004	1	1	0	1	1	0	0	16.442	16.442	31.8799	0	PROCESSED	57605.7438078704	2016-08-05 17:51:05	56582	2013-10-17 00:00:00	56219.6572916667	2012-10-19 15:46:30	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072014	We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed.	GALACTIC DIFFUSE EMISSION	5	A	TOBIAS PRINZ		EUR	7	AO7	IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507067010/	Quick Look
411	GRXE_E_4	267.9068	-26.8159	267.125467	-26.803832	268.119163	-3.388548	2.50111874	-0.04382328	104.4995	56371.1118518518	2013-03-20 02:41:04	56373.3049421296	2013-03-22 07:19:07	507071010	101.2086	100	101.2166	101.2086	0	101.2166	2	2	0	2	1	0	0	105.6491	105.6491	189.4519	1	PROCESSED	57610.9065625	2016-08-10 21:45:27	56018	2012-04-01 00:00:00	56384.6094560185	2013-04-02 14:37:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507071010/	Quick Look
412	COMET_8P_TUTTLE-P2_09	40.126	-36.804	39.619449	-37.017725	21.006365	-49.022029	242.56232387	-65.03879756	253.3121	54491.0963773148	2008-01-26 02:18:47	54491.2292824074	2008-01-26 05:30:10	502063090	4.3979	4	4.3979	4.3979	0	4.3979	1	1	0	1	1	0	0	4.752	4.752	11.4439	0	PROCESSED	57541.402662037	2016-06-02 09:39:50	54912	2009-03-22 00:00:00	54546.2142592593	2008-03-21 05:08:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063090/	Quick Look
413	W44_NORTH	283.9599	1.4928	283.326032	1.427124	285.320102	24.193967	34.76225024	-0.29835298	254.9998	56584.8902083333	2013-10-19 21:21:54	56586.2084837963	2013-10-21 05:00:13	508005010	55.6459	60	55.7019	55.6459	0	55.7008	1	1	0	1	1	0	0	47.4531	47.4531	113.8958	1	PROCESSED	57613.0578356482	2016-08-13 01:23:17	56967	2014-11-06 00:00:00	56597.6717824074	2013-11-01 16:07:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080012	W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	8	AO8	MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508005010/	Quick Look
414	HESS J1534-571 4	233.6872	-56.8979	232.705572	-56.731059	246.296725	-36.40404	323.85352453	-0.81317458	295.9989	56545.1801157407	2013-09-10 04:19:22	56545.8042708333	2013-09-10 19:18:09	508016010	42.1696	40	42.1696	42.1936	0	42.1776	2	2	0	2	1	0	0	39.9419	39.9419	53.9199	0	PROCESSED	57612.5878587963	2016-08-12 14:06:31	56990	2014-11-29 00:00:00	56625.6134953704	2013-11-29 14:43:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080024	Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	8	AO8	RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508016010/	Quick Look
415	G355.6-0.0	263.7798	-32.6083	262.962219	-32.576152	264.68406	-9.281685	355.69106204	-0.03789327	90.0013	55246.5249074074	2010-02-19 12:35:52	55247.6293287037	2010-02-20 15:06:14	504098010	52.5044	50	52.5275	52.5204	0	52.5044	2	2	0	2	1	0	0	43.7346	43.7346	95.4118	0	PROCESSED	57550.6569560185	2016-06-11 15:46:01	54922	2009-04-01 00:00:00	55257.1119444444	2010-03-02 02:41:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504098010/	Quick Look
416	G21.5-0.9	278.4038	-10.5066	277.711815	-10.545632	278.460388	12.687474	21.56207071	-0.86897985	103.5553	54190.0674074074	2007-03-31 01:37:04	54191.7405671296	2007-04-01 17:46:25	502065020	53.5261	100	53.5261	53.551	0	53.5661	1	2	0	1	1	0	0	48.618	48.618	144.5418	0	PROCESSED	57538.0817013889	2016-05-30 01:57:39	54695	2008-08-17 00:00:00	54200.5054861111	2007-04-10 12:07:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021211	We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray.	GALACTIC DIFFUSE EMISSION	5	B	ILANA HARRUS		USA	2	AO2	SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502065020/	Quick Look
417	JUPITER	103.7993	23.1163	103.042955	23.180911	102.674134	0.280458	192.50244401	11.09547038	264.3793	56762.0858912037	2014-04-15 02:03:41	56762.3890277778	2014-04-15 09:20:12	508023010	13.0905	160	13.0905	13.0905	0	13.0905	1	1	0	1	1	0	0	13.005	13.005	26.1839	0	PROCESSED	57614.2446527778	2016-08-14 05:52:18	57212	2015-07-09 00:00:00	56778.6117708333	2014-05-01 14:40:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023010/	Quick Look
418	JUPITER	104.0402	23.0972	103.284076	23.16295	102.896521	0.28265	192.61518388	11.28841687	264.4641	56764.0628125	2014-04-17 01:30:27	56764.1911805556	2014-04-17 04:35:18	508023070	4.5577	160	4.5577	4.5577	0	4.5737	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57614.9502777778	2016-08-14 22:48:24	57212	2015-07-09 00:00:00	56782.4904976852	2014-05-05 11:46:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023070/	Quick Look
419	JUPITER	104.5088	23.0594	103.753114	23.127361	103.329251	0.287317	192.8346306	11.66394816	267.1301	56767.4497106482	2014-04-20 10:47:35	56767.7814583333	2014-04-20 18:45:18	508023120	11.1894	160	11.1894	11.1961	0	11.1974	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57614.962974537	2016-08-14 23:06:41	57212	2015-07-09 00:00:00	56789.8021759259	2014-05-12 19:15:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023120/	Quick Look
420	RCW86_SE	221.3859	-62.671	220.394052	-62.460463	241.394031	-43.97094	315.61056381	-2.64231092	96.79	54863.365787037	2009-02-01 08:46:44	54864.7550115741	2009-02-02 18:07:13	503004010	53.3274	50	53.3594	53.3274	0	53.3594	2	2	0	2	1	0	0	47.8136	47.8136	119.9879	0	PROCESSED	57545.4381481482	2016-06-06 10:30:56	55329	2010-05-13 00:00:00	54880.5420138889	2009-02-18 13:00:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030011	Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		JAP	3	AO3	RCW86 MAPPING OBSERVATION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503004010/	Quick Look
421	GC_LARGEPROJECT4	266.0398	-29.5556	265.241679	-29.534433	266.526203	-6.162189	359.30535174	-0.05184233	261.05	54715.6640393518	2008-09-06 15:56:13	54717.0690277778	2008-09-08 01:39:24	503010010	53.1056	50	53.1216	53.1056	0	53.1136	2	2	0	2	1	0	0	37.0646	37.0646	121.366	1	PROCESSED	57543.7725694444	2016-06-04 18:32:30	54557	2008-04-01 00:00:00	54780.6585648148	2008-11-10 15:48:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503010010/	Quick Look
422	VELA PWN W2	127.3498	-45.1919	126.932022	-45.023781	151.542711	-60.896813	262.94388066	-3.64107383	303.5006	56439.0351851852	2013-05-27 00:50:40	56439.4696643518	2013-05-27 11:16:19	508043010	19.5844	15	19.5924	19.5844	0	19.6004	2	2	0	2	1	0	0	15.6266	15.6266	37.5339	1	PROCESSED	57611.391875	2016-08-11 09:24:18	56816	2014-06-08 00:00:00	56450.7935532407	2013-06-07 19:02:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080090	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered.	GALACTIC DIFFUSE EMISSION	5	B	KOJI MORI		JAP	8	AO8	SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508043010/	Quick Look
423	GC_LARGEPROJECT10	264.8736	-31.1751	264.065254	-31.148261	265.564785	-7.81275	357.39875369	-0.05245192	268.5898	54731.2832060185	2008-09-22 06:47:49	54732.3383912037	2008-09-23 08:07:17	503016010	52.1712	50	52.1712	52.1792	0	52.1792	2	2	0	2	1	0	0	49.2913	49.2913	91.1639	1	PROCESSED	57543.9863425926	2016-06-04 23:40:20	54557	2008-04-01 00:00:00	54780.6078935185	2008-11-10 14:35:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503016010/	Quick Look
424	VELA PWN W3	126.9052	-45.2087	126.488861	-45.042306	150.998783	-61.06652	262.77480933	-3.90558145	95.0008	56590.9784606482	2013-10-25 23:28:59	56591.4343055556	2013-10-26 10:25:24	508044010	13.871	15	13.871	13.871	0	13.871	2	2	0	2	1	0	0	11.3448	11.3448	39.3799	1	PROCESSED	57613.1197106482	2016-08-13 02:52:23	57009	2014-12-18 00:00:00	56643.6595949074	2013-12-17 15:49:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080090	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered.	GALACTIC DIFFUSE EMISSION	5	B	KOJI MORI		JAP	8	AO8	SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508044010/	Quick Look
425	GC_LARGEPROJECT15	265.2338	-30.2129	264.431646	-30.187819	265.84334	-6.840443	358.37855715	0.19604348	267.777	54743.1555902778	2008-10-04 03:44:03	54744.4565277778	2008-10-05 10:57:24	503021010	53.826	50	53.834	53.834	0	53.826	2	2	0	2	1	0	0	49.6405	49.6405	112.3781	0	PROCESSED	57544.0429861111	2016-06-05 01:01:54	54557	2008-04-01 00:00:00	54780.430150463	2008-11-10 10:19:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503021010/	Quick Look
426	SGR A	266.5133	-28.9285	265.71907	-28.909638	266.925006	-5.524591	0.05589981	-0.0769322	266.9997	56555.4484490741	2013-09-20 10:45:46	56556.6446875	2013-09-21 15:28:21	508064010	50.4569	50	50.4569	50.4569	0	50.4569	2	2	0	2	1	0	0	45.2248	45.2248	103.308	0	PROCESSED	57612.6971527778	2016-08-12 16:43:54	56956	2014-10-26 00:00:00	56588.757025463	2013-10-23 18:10:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080143	X-ray emissions from giant molecular clouds (X-ray reflection nebula) in the Galactic center region show past activity of the super-massive black hole, Sagittarius (Sgr) A. Using Suzaku, we have found that Sgr A had been in the active phase for almost a thousand years and dropped down to the quiescent level tens of years ago. However, no detailed information during the active phase and transition has been obtained from observations to study a mechanism of the sudden phase change. We aim to observe new information about time variability and relative positions from X-ray reflection nebulae to find the past light curve of Sgr A*. This work will be the grand sum for the Suzaku observation of the Galactic center.	GALACTIC DIFFUSE EMISSION	5	A	MASAYOSHI NOBUKAWA	YOSHITOMO MAEDA	JAP	8	AO8	PAST HISTORY OF THE SUPER-MASSIVE BLACK HOLE IN THE GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508064010/	Quick Look
427	0509-67.5	77.4191	-67.5347	77.43679	-67.59534	342.967322	-85.012032	278.15520093	-34.57404921	36.9172	56491.0670601852	2013-07-18 01:36:34	56495.4689583333	2013-07-22 11:15:18	508072020	152.6517	150	152.6997	152.6517	0	152.6997	2	2	0	2	1	0	0	139.7536	139.7536	380.2994	7	PROCESSED	57612.009537037	2016-08-12 00:13:44	56383	2013-04-01 00:00:00	56509.8769097222	2013-08-05 21:02:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081315	We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		USA	8	AO8	LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508072020/	Quick Look
428	MBM36	238.3604	-4.7951	237.700156	-4.647695	237.207526	15.116261	4.00027103	35.69642682	294.5973	56525.2685300926	2013-08-21 06:26:41	56526.5655092593	2013-08-22 13:34:20	508079010	49.6555	80	49.6555	49.6555	0	49.6555	2	2	0	2	1	0	0	42.8799	42.8799	112.0458	2	PROCESSED	57612.3808912037	2016-08-12 09:08:29	56383	2013-04-01 00:00:00	56587.6359027778	2013-10-22 15:15:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086002	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	8	AO8	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508079010/	Quick Look
429	HESS_J1825-137_2	276.1969	-13.7002	275.488545	-13.728547	276.096187	9.609358	17.73170044	-0.43977824	271.0001	54756.4591666667	2008-10-17 11:01:12	54758.1953009259	2008-10-19 04:41:14	503029010	57.1993	50	57.1993	57.1993	0	57.1993	2	2	0	2	1	0	0	51.185	51.185	149.9858	0	PROCESSED	57544.2276157407	2016-06-05 05:27:46	55148	2009-11-13 00:00:00	54780.5081365741	2008-11-10 12:11:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030044	The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons.	GALACTIC DIFFUSE EMISSION	5	B	TAKAAKI TANAKA		JAP	3	AO3	MAPPING OBSERVATIONS OF HESS J1825-137	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503029010/	Quick Look
430	HESSJ1614-A	243.5214	-52.1022	242.56254	-51.975946	251.486678	-30.347435	331.29897546	-0.76107386	283.3889	54729.7629050926	2008-09-20 18:18:35	54730.562662037	2008-09-21 13:30:14	503073010	53.6494	50	53.6574	53.6494	0	53.6654	1	1	0	1	1	0	0	40.8713	40.8713	69.0719	0	PROCESSED	57543.9752662037	2016-06-04 23:24:23	55148	2009-11-13 00:00:00	54780.4246990741	2008-11-10 10:11:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030088	The TeV image of HESSJ1614-518 is double peaked, and we observed one of them during the AO-1 with the Suzaku XIS. We discovered extended X-ray emission which coincides with the TeV emission. Then we propose to observe the other peak. We also found a bright object between the double peaks. HESSJ1614 may be a pulsar wind nebula, and the object may be a pulsar driving the nebula. However, the object was just at the edge of the XIS field of view, we could not study it in detail. Then, we propose another position to observe the object. Furthermore, we discovered soft diffuse emission around HESSJ1614. We propose the other position to study the spatial extension of the diffuse emission.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	3	AO3	MAPPING OBSERVATION OF HESSJ1614-518	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503073010/	Quick Look
431	HESSJ1832	278.156	-8.4222	277.474303	-8.460064	278.335703	14.782649	23.29856204	0.30967904	88.1963	55659.2543518518	2011-04-08 06:06:16	55660.3454282407	2011-04-09 08:17:25	506021010	40.3432	40	40.3432	40.3432	0	40.3432	2	2	0	2	1	0	0	34.8513	34.8513	94.2578	1	PROCESSED	57601.464224537	2016-08-01 11:08:29	56043	2012-04-26 00:00:00	55673.2950925926	2011-04-22 07:04:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060061	Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	6	AO6	ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506021010/	Quick Look
432	MBM20	68.9307	-14.6229	68.358009	-14.724304	64.461829	-36.216174	211.39181931	-36.56844204	64.9904	56520.8174074074	2013-08-16 19:37:04	56522.5001967593	2013-08-18 12:00:17	508081010	56.4905	80	56.4905	56.4905	0	56.4905	2	2	0	2	1	0	0	55.086	55.086	145.38	1	PROCESSED	57612.3311111111	2016-08-12 07:56:48	56383	2013-04-01 00:00:00	56587.6432291667	2013-10-22 15:26:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086002	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	8	AO8	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508081010/	Quick Look
433	CYGNUS LOOP (P25)	311.8608	32.1678	311.350497	31.982956	327.005863	47.670937	74.68970828	-7.03578766	60.8878	54621.6278472222	2008-06-04 15:04:06	54622.1488888889	2008-06-05 03:34:24	503061010	25.9959	20	25.9959	25.9959	0	25.9959	2	2	0	2	1	0	0	23.8791	23.8791	45.01	0	PROCESSED	57542.7242476852	2016-06-03 17:22:55	55003	2009-06-21 00:00:00	54636.2508217593	2008-06-19 06:01:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503061010/	Quick Look
434	VELA PWN GEV3	128.0196	-44.9062	127.597638	-44.735505	152.091567	-60.413918	262.99085627	-3.09029782	119.9755	56986.5006481482	2014-11-25 12:00:56	56986.9105439815	2014-11-25 21:51:11	509013010	18.4893	15	18.4893	18.4969	0	18.4893	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.8178009259	2016-08-16 19:37:38	57366	2015-12-10 00:00:00	57002.4411226852	2014-12-11 10:35:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090046	We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	9	AO9	X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509013010/	Quick Look
435	VELA PWN GEV4	127.5996	-44.9062	127.17888	-44.73712	151.566964	-60.561222	262.81539743	-3.33071285	121.1346	56986.9114814815	2014-11-25 21:52:32	56987.558587963	2014-11-26 13:24:22	509014010	17.9817	15	17.9817	17.9897	0	17.9977	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.8244328704	2016-08-16 19:47:11	57368	2015-12-12 00:00:00	57002.4392824074	2014-12-11 10:32:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090046	We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	9	AO9	X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509014010/	Quick Look
436	G166.0+4.3_NE	81.7715	42.9863	80.874617	42.944315	83.616156	19.728231	166.13139999	4.39632756	84.8097	56922.0215740741	2014-09-22 00:31:04	56923.3544444444	2014-09-23 08:30:24	509022020	58.5598	60	58.5598	61.5039	0	61.4879	2	2	0	2	1	0	0	2.207	2.207	5.696	0	PROCESSED	57616.5872685185	2016-08-16 14:05:40	57312	2015-10-17 00:00:00	56945.1963657407	2014-10-15 04:42:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090092	Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation.	GALACTIC DIFFUSE EMISSION	5	A	AKIHIRO TAKATA		JAP	9	AO9	G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509022020/	Quick Look
437	CIZA J1358.9-4750_NW	209.4473	-47.6057	208.659126	-47.362265	225.512998	-33.070935	314.36323033	13.78794346	293.0002	56880.8612615741	2014-08-11 20:40:13	56881.8265972222	2014-08-12 19:50:18	509028010	41.501	40	41.501	41.525	0	41.509	2	2	0	2	1	0	0	7.9918	7.9918	20.64	0	PROCESSED	57616.4817939815	2016-08-16 11:33:47	57267	2015-09-02 00:00:00	56898.4888657407	2014-08-29 11:43:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090102	Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS.	GALACTIC DIFFUSE EMISSION	5	B	YUICHI KATO		JAP	9	AO9	OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509028010/	Quick Look
438	G189 EAST	95.4705	22.4826	94.715097	22.507311	95.056054	-0.862354	189.63783855	3.93426331	258.2106	57096.5099652778	2015-03-15 12:14:21	57098.6780324074	2015-03-17 16:16:22	509036010	66.0529	85	66.0529	86.2237	0	86.2397	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8236226852	2016-08-17 19:46:01	57524	2016-05-16 00:00:00	57157.5685416667	2015-05-15 13:38:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091314	We propose observations of G189.6+3.3, a large candidate supernova remnant (SNR) that overlaps with the much better studied remnant IC 443. Little is known about G189; ROSAT images show a shell-like structure about 1.5$^{circ}$ in diameter, but it has never been observed with modern X-ray telescopes. Its association, or lack thereof, with IC 443 is unknown. It may not be a supernova remnant at all; a superbubble origin for the X-ray emission also provides an intriguing possibility. Spatially-resolved spectroscopy with Suzaku will allow the detailed measurement of the plasma properties, illuminating the nature of this object. Determining the nature of G189 will help to probe the evolution of the ISM driven by the deaths of massive stars.	GALACTIC DIFFUSE EMISSION	5	B	BRIAN WILLIAMS		USA	9	AO9	OBSERVATIONS OF G189.6+3.3: AN SNR COMPANION TO IC 443?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509036010/	Quick Look
439	RADIO_ARC_SOUTH	266.9853	-29.0688	266.190093	-29.052225	267.342882	-5.6555	0.15000746	-0.5026703	267.1998	56186.0290509259	2012-09-16 00:41:50	56188.8203472222	2012-09-18 19:41:18	507016010	103.472	100	103.472	103.472	0	103.472	2	2	0	2	1	0	0	89.1906	89.1906	241.1319	4	PROCESSED	57607.146875	2016-08-07 03:31:30	56668	2014-01-11 00:00:00	56303.6234490741	2013-01-11 14:57:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070016	The 6.4 keV emission associated with giant molecular clouds is the most prominent feature in the Galactic center region. So far, the origin has only been found and discussed in the X-ray reflection process. We propose deep observation at the Radio Arc to discover the 6.4 keV emission in the particle origin, which would open the window to study the nature of the Galactic cosmic ray.	GALACTIC DIFFUSE EMISSION	5	A	SYUKYO RYU		JAP	7	AO7	X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN --	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507016010/	Quick Look
440	VELA JR SE1	133.9641	-46.7818	133.536852	-46.589245	161.150153	-59.841767	267.02895458	-1.00032542	109.9994	56621.589525463	2013-11-25 14:08:55	56622.3175462963	2013-11-26 07:37:16	508060010	40.5996	40	40.5996	40.5996	0	40.6057	2	2	0	2	1	0	0	46.6535	46.6535	62.8959	0	PROCESSED	57613.4271990741	2016-08-13 10:15:10	56998	2014-12-07 00:00:00	56632.5928240741	2013-12-06 14:13:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080117	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr.	GALACTIC DIFFUSE EMISSION	5	C	TARO FUKUYAMA		JAP	8	AO8	OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR.	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508060010/	Quick Look
441	KES 69	278.2575	-10.136	277.567341	-10.174332	278.335469	13.065931	21.8245316	-0.57033928	267.6495	56927.2830902778	2014-09-27 06:47:39	56929.1391435185	2014-09-29 03:20:22	509037010	77.3795	80	77.3795	77.9708	0	77.9953	2	2	0	3	0	0	0	0	0	0	0	PROCESSED	57616.5892361111	2016-08-16 14:08:30	57345	2015-11-19 00:00:00	56979.4056944444	2014-11-18 09:44:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091315	We propose to conduct Suzaku observations of the Galactic supernova remnants (SNRs) Kes 69 (G21.8-0.6) and 3C 396 (G39.2-0.3). These SNRs were detected in the infrared by Spitzer and their infrared colors suggest that shocked molecules produce the observed emission. Published analyses of the X-ray emission from these SNRs (along with our own analysis of archival XMM-Newton and Chandra observations of these sources) reveals that the emission from both Kes 69 and 3C 396 is thermal and that they may both be mixed-morphology SNRs (MMSNRs) but deeper observations are needed to clarify their X-ray spectral properties. In particular, we will investigate whether these X-ray emitting plasmas are overionized, which is observed for other MMSNRs.	GALACTIC DIFFUSE EMISSION	5	A	THOMAS PANNUTI		USA	9	AO9	SUZAKU OBSERVATIONS OF THE SPITZER-DETECTED GALACTIC SUPERNOVA REMNANTS KES 69 (G21.8-0.6) AND 3C 396 (G39.2-0.3)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509037010/	Quick Look
442	RXJ1713-3946_ID1	257.9616	-39.5166	257.09684	-39.456462	260.331165	-16.477991	347.33828294	-0.06271892	87.0007	55242.129375	2010-02-15 03:06:18	55243.2502199074	2010-02-16 06:00:19	504027010	61.5331	60	61.5578	61.5331	0	61.5738	3	2	0	2	1	0	0	46.7259	46.7259	96.8238	0	PROCESSED	57550.6101273148	2016-06-11 14:38:35	55622	2011-03-02 00:00:00	55253.4734259259	2010-02-26 11:21:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040021	We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009.	GALACTIC DIFFUSE EMISSION	5	B	TADAYUKI TAKAHASHI		JAP	4	AO4	STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504027010/	Quick Look
443	FERMI_JET_COCOON_2	320.2279	-29.504	319.485138	-29.716859	313.416673	-13.31861	17.00065384	-44.00205209	255.063	56981.4053356482	2014-11-20 09:43:41	56981.8683217593	2014-11-20 20:50:23	509048010	19.9032	20	19.9032	19.9032	0	19.9032	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7951736111	2016-08-16 19:05:03	57362	2015-12-06 00:00:00	56995.5937268518	2014-12-04 14:14:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091322	The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way.	GALACTIC DIFFUSE EMISSION	5	C	MATTHEW MILLER		USA	9	AO9	OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509048010/	Quick Look
444	DIFFUSE1E	200.6072	7.3824	199.979251	7.643505	196.163547	14.87503	324.76377809	68.9302329	123.5311	57011.0086458333	2014-12-20 00:12:27	57011.5252083333	2014-12-20 12:36:18	509062010	23.9762	20	23.9762	24.5362	0	24.5362	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.5495023148	2016-08-17 13:11:17	57475	2016-03-28 00:00:00	57107.4289583333	2015-03-26 10:17:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091324	In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them.	GALACTIC DIFFUSE EMISSION	5	C	JOEL BREGMAN		USA	9	AO9	UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509062010/	Quick Look
445	MBM16	49.7641	11.5835	49.080496	11.40241	50.44037	-6.504342	170.59835317	-37.27294118	77.8263	56867.2632638889	2014-07-29 06:19:06	56869.0606018518	2014-07-31 01:27:16	509073010	78.81	80	78.818	78.818	0	78.81	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.4583449074	2016-08-16 11:00:01	56748	2014-04-01 00:00:00	56902.6996180556	2014-09-02 16:47:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096001	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	9	AO9	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509073010/	Quick Look
446	VELA FRAGMENT C	136.2696	-44.691	135.819541	-44.490549	161.57955	-57.213344	266.51473212	1.58715492	269.3614	54580.6978703704	2008-04-24 16:44:56	54582.3056481482	2008-04-26 07:20:08	503095010	84.1167	70	84.1167	84.1167	0	84.1167	2	2	0	2	1	0	0	91.3547	91.3547	138.9018	2	PROCESSED	57542.4305439815	2016-06-03 10:19:59	54960	2009-05-09 00:00:00	54594.2480324074	2008-05-08 05:57:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031212	Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM.	GALACTIC DIFFUSE EMISSION	5	B	TERRANCE GAETZ		USA	3	AO3	SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503095010/	Quick Look
447	GB_NORTH_1	266.1004	-28.3619	265.30982	-28.341045	266.546613	-4.967513	0.35022505	0.52781175	106.0661	57104.6393981482	2015-03-23 15:20:44	57106.6752777778	2015-03-25 16:12:24	509077010	98.2407	100	98.2407	98.4407	0	98.4407	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8715277778	2016-08-17 20:55:00	56748	2014-04-01 00:00:00	57120.4153125	2015-04-08 09:58:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096002	The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	9	AO9	MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY-	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509077010/	Quick Look
448	HESS J1745-303A	265.7791	-30.3241	264.976083	-30.301658	266.320995	-6.936807	358.53258375	-0.26269922	103.33	55253.3854166667	2010-02-26 09:15:00	55254.6758796296	2010-02-27 16:13:16	504001010	51.1538	50	51.1618	51.1538	0	51.1685	2	2	0	2	1	0	0	42.2196	42.2196	111.4581	1	PROCESSED	57550.7381134259	2016-06-11 17:42:53	55636	2011-03-16 00:00:00	55267.2568634259	2010-03-12 06:09:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040001	The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	4	AO4	DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504001010/	Quick Look
449	RADIO_ARC_S_E	267.1914	-28.7693	266.398054	-28.753729	267.517971	-5.352408	0.49965543	-0.50260843	267.4999	56199.7928125	2012-09-29 19:01:39	56200.9349652778	2012-09-30 22:26:21	507017010	54.1782	50	54.2022	54.1782	0	54.202	1	1	0	1	1	0	0	51.7936	51.7936	98.6799	0	PROCESSED	57607.2277777778	2016-08-07 05:28:00	56592	2013-10-27 00:00:00	56226.621400463	2012-10-26 14:54:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070016	The 6.4 keV emission associated with giant molecular clouds is the most prominent feature in the Galactic center region. So far, the origin has only been found and discussed in the X-ray reflection process. We propose deep observation at the Radio Arc to discover the 6.4 keV emission in the particle origin, which would open the window to study the nature of the Galactic cosmic ray.	GALACTIC DIFFUSE EMISSION	5	A	SYUKYO RYU		JAP	7	AO7	X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN --	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507017010/	Quick Look
450	BLOWOUT2	311.9515	31.5359	311.437845	31.350733	326.744585	47.059417	74.23825049	-7.48819964	243.427	55158.9662615741	2009-11-23 23:11:25	55159.5106944444	2009-11-24 12:15:24	504012010	26.5494	23	26.5654	26.5494	0	26.5734	1	1	0	1	1	0	0	19.9401	19.9401	47.0319	1	PROCESSED	57549.5397800926	2016-06-10 12:57:17	55545	2010-12-15 00:00:00	55176.2336921296	2009-12-11 05:36:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504012010/	Quick Look
451	W49B	287.7847	9.1153	287.186342	9.031642	290.654992	31.289584	43.2812159	-0.18378496	89.2674	54921.5302662037	2009-03-31 12:43:35	54923.0613425926	2009-04-02 01:28:20	504035010	61.7825	100	61.7905	61.7845	0	61.7825	3	3	0	3	1	0	0	55.1556	55.1556	132.2739	3	PROCESSED	57546.0146412037	2016-06-07 00:21:05	55324	2010-05-08 00:00:00	54949.4493287037	2009-04-28 10:47:02	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040075	Observation of the W49B supernova remnant for 100 ksec is proposed to detect Ti emission line at the 3 sigma confidence level. In order to reveal whether it is a remnant of Type Ia supernova or not, detailed measurement of the rare metal elements such as Cr, Mn, Ni, and Ti is essential. We determine the type by Ti to Cr, Mn to Cr, and Ni to Fe ratios. Furthermore, we investigate whether its plasma is in the overionized status or not.	GALACTIC DIFFUSE EMISSION	5	B	MIDORI OZAWA		JAP	4	AO4	UNMASK THE NATURE OF W49B !	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504035010/	Quick Look
452	FESI2	313.183	30.3797	312.661298	30.190122	327.500793	45.583083	73.99193661	-9.03499466	225.2405	55174.9860300926	2009-12-09 23:39:53	55175.7904398148	2009-12-10 18:58:14	504018010	34.5904	34	34.5904	34.5904	0	34.5904	2	2	0	2	1	0	0	30.318	30.318	69.4939	0	PROCESSED	57549.7573032407	2016-06-10 18:10:31	55555	2010-12-25 00:00:00	55189.1622916667	2009-12-24 03:53:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504018010/	Quick Look
453	GALACTIC_BULGE7	266.6764	-30.8281	265.869887	-30.809998	267.112733	-7.42025	358.50617228	-1.18471698	274.4326	55117.1787037037	2009-10-13 04:17:20	55118.4785416667	2009-10-14 11:29:06	504090010	41.2607	50	41.2607	52.9033	0	52.9033	3	2	0	2	1	0	0	34.964	34.964	112.2938	2	PROCESSED	57548.8825694444	2016-06-09 21:10:54	54922	2009-04-01 00:00:00	55133.2421643518	2009-10-29 05:48:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504090010/	Quick Look
454	HESS J1809-193B	272.6789	-19.1585	271.941455	-19.169725	272.527802	4.258732	11.32661741	-0.06027609	269.0544	55084.4838773148	2009-09-10 11:36:47	55085.7488310185	2009-09-11 17:58:19	504078010	52.4748	50	52.4748	52.4748	0	52.4748	2	2	0	2	1	0	0	43.3733	43.3733	109.2758	1	PROCESSED	57548.5486226852	2016-06-09 13:10:01	55475	2010-10-06 00:00:00	55109.4280555556	2009-10-05 10:16:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041303	We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background.	GALACTIC DIFFUSE EMISSION	5	A	OLEG KARGALTSEV		USA	4	AO4	CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504078010/	Quick Look
455	330.2+1.0	240.2384	-51.525	239.295706	-51.384773	249.047523	-30.224565	330.18352169	1.02987491	98.9027	55239.832025463	2010-02-12 19:58:07	55242.125150463	2010-02-15 03:00:13	504083030	92.505	30	92.513	92.505	0	92.521	2	2	0	2	1	0	0	86.0965	86.0965	198.0897	4	PROCESSED	57550.6564699074	2016-06-11 15:45:19	55622	2011-03-02 00:00:00	55253.5397685185	2010-02-26 12:57:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041312	Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity.	GALACTIC DIFFUSE EMISSION	5	B	GLENN ALLEN		USA	4	AO4	MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504083030/	Quick Look
456	3C_397	286.9038	7.1223	286.296185	7.042755	289.336416	29.435283	41.11064468	-0.32936267	256.5108	55493.8258449074	2010-10-24 19:49:13	55495.8022337963	2010-10-26 19:15:13	505008010	69.3266	70	69.3266	69.3266	0	69.3266	2	2	0	2	1	0	0	62.1653	62.1653	170.7319	0	PROCESSED	57553.8922800926	2016-06-14 21:24:53	55287	2010-04-01 00:00:00	55505.3393981482	2010-11-05 08:08:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050002	We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505008010/	Quick Look
457	CYGNUS LOOP 5	312.0188	31.9594	311.507127	31.773986	327.066622	47.426634	74.60885135	-7.27014396	81.8368	55305.8645833333	2010-04-19 20:45:00	55306.4578125	2010-04-20 10:59:15	505013010	26.8452	26	26.8452	26.8452	0	26.8452	1	1	0	1	1	0	0	21.277	21.277	51.232	2	PROCESSED	57551.2602083333	2016-06-12 06:14:42	55287	2010-04-01 00:00:00	55364.2036458333	2010-06-17 04:53:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505013010/	Quick Look
458	CYGNUS LOOP 11	313.8693	30.5587	313.347105	30.366695	328.378211	45.516461	74.51088669	-9.3807208	82.002	55328.698587963	2010-05-12 16:45:58	55329.1251736111	2010-05-13 03:00:15	505019010	18.8976	18	18.9056	18.8976	0	18.9136	2	2	0	2	1	0	0	14.9048	14.9048	36.8539	1	PROCESSED	57551.490150463	2016-06-12 11:45:49	55287	2010-04-01 00:00:00	55393.3619791667	2010-07-16 08:41:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505019010/	Quick Look
459	WESTERLUND1_4	253.5509	-45.3005	252.641306	-45.219522	257.53427	-22.567529	340.7711384	-1.01287357	288.2868	55463.3974652778	2010-09-24 09:32:21	55464.5203587963	2010-09-25 12:29:19	505052010	49.627	50	49.627	49.627	0	49.627	2	2	0	2	1	0	0	40.2137	40.2137	97.0079	1	PROCESSED	57553.5510416667	2016-06-14 13:13:30	55840	2011-10-06 00:00:00	55474.1080208333	2010-10-05 02:35:33	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050078	TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster.	GALACTIC DIFFUSE EMISSION	5	A	HIRONORI MATSUMOTO		JAP	5	AO5	IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505052010/	Quick Look
460	VELA SNR CB-LBG	130.6266	-44.6167	130.194556	-44.436193	154.988854	-59.23497	263.87788945	-1.43970243	293.482	55319.3460648148	2010-05-03 08:18:20	55319.7940046296	2010-05-03 19:03:22	505071010	27.1799	20	27.1799	27.1799	0	27.1799	2	2	0	2	1	0	0	25.0945	25.0945	38.6939	1	PROCESSED	57551.3691203704	2016-06-12 08:51:32	55696	2011-05-15 00:00:00	55330.1543981482	2010-05-14 03:42:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051304	The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	5	AO5	IRON-RICH EJECTA BULLET IN THE VELA SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505071010/	Quick Look
461	GALACTIC_BULGE4	269.1417	-30.4015	268.337633	-30.395373	269.244618	-6.962713	359.95546853	-2.79264334	69.3552	55632.2752314815	2011-03-12 06:36:20	55633.4287152778	2011-03-13 10:17:21	505079010	50.2193	50	50.2273	50.2193	0	50.2273	2	2	0	2	1	0	0	43.375	43.375	99.648	1	PROCESSED	57601.1540277778	2016-08-01 03:41:48	55287	2010-04-01 00:00:00	55645.5706134259	2011-03-25 13:41:41	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505079010/	Quick Look
462	GALACTIC_BULGE5	270.1525	-30.903	269.345086	-30.901777	270.122341	-7.462063	359.95222621	-3.79644913	86.7823	55293.7188657407	2010-04-07 17:15:10	55295.8849074074	2010-04-09 21:14:16	505080010	56.1396	50	56.1396	56.1396	0	56.1396	2	2	0	2	1	0	0	55.1498	55.1498	185.0058	1	PROCESSED	57553.0630439815	2016-06-14 01:30:47	55287	2010-04-01 00:00:00	55441.4355555556	2010-09-02 10:27:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505080010/	Quick Look
463	JUPITER	29.0345	10.6283	28.369064	10.38411	30.736601	-1.177073	147.65759499	-49.11229838	249.1849	55938.2087962963	2012-01-12 05:00:40	55939.2481944444	2012-01-13 05:57:24	506006040	38.6289	160	38.6289	38.6367	0	38.6369	2	2	0	2	1	0	0	31.7692	31.7692	89.7859	0	PROCESSED	57604.3463657407	2016-08-04 08:18:46	56388	2013-04-06 00:00:00	56020.1680208333	2012-04-03 04:01:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060017	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter.	GALACTIC DIFFUSE EMISSION	5	B	KUMI ISHIKAWA		JAP	6	AO6	STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006040/	Quick Look
464	THE KEPLER SNR	262.6707	-21.4823	261.92146	-21.444975	263.169631	1.785142	4.52498329	6.82417088	98.3356	55620.8079166667	2011-02-28 19:23:24	55624.797337963	2011-03-04 19:08:10	505092040	146.2337	250	146.2337	146.2541	0	146.2577	2	2	0	2	1	0	0	113.8022	113.8022	344.6577	6	PROCESSED	57601.192337963	2016-08-01 04:36:58	55287	2010-04-01 00:00:00	55642.4090046296	2011-03-22 09:48:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092040/	Quick Look
465	CYGNUS LOOP BLOWOUT1	312.1499	29.2487	311.624762	29.062833	325.710057	44.881262	72.53069275	-9.03908096	78.1532	55686.7775578704	2011-05-05 18:39:41	55687.8494907407	2011-05-06 20:23:16	506011010	48.5641	50	48.5641	48.5641	0	48.5641	2	2	0	2	1	0	0	42.0429	42.0429	92.5799	1	PROCESSED	57601.954224537	2016-08-01 22:54:05	56066	2012-05-19 00:00:00	55698.3278472222	2011-05-17 07:52:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060053	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	6	AO6	MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506011010/	Quick Look
466	GAMMACYGNI_NWSHELL2	304.652	40.6975	304.208167	40.540107	324.021819	57.820534	78.12229495	2.68416641	82.9982	55665.3027430556	2011-04-14 07:15:57	55666.2688657407	2011-04-15 06:27:10	506018010	39.712	40	39.712	39.712	0	39.712	2	2	0	2	1	0	0	36.1165	36.1165	83.4379	0	PROCESSED	57601.5048032407	2016-08-01 12:06:55	56058	2012-05-11 00:00:00	55690.9818402778	2011-05-09 23:33:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060059	We propose deep X-ray observations of outer edge of gamma Cygni SNR north-west shell with Suzaku. Radio observation shows that this SNR has shell-type structure in the north-west and south-east. High energy diffuse gamma-ray emission have been recently detected from the north-west shell by Fermi gamma-ray space telescope and VERITAS TeV telescope. Main objective of this proposal is to reveal the emission mechanisms not only in X-ray band but also in GeV and TeV bands through the extent of the X-ray emission and spectroscopy. Only Suzaku can achieve this, because the background level of XIS is very low and the broadness of the energy band.	GALACTIC DIFFUSE EMISSION	5	B	YASUYUKI TANAKA		JAP	6	AO6	SUZAKU X-RAY OBSERVATION OF OUTER EDGE OF GAMMA CYGNI SNR NORTH-WEST SHELL	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506018010/	Quick Look
467	S147_N	87.0463	27.5187	86.260987	27.502453	87.375766	4.104837	181.50494456	-0.25223067	273.8998	55997.2930324074	2012-03-11 07:01:58	55998.555787037	2012-03-12 13:20:20	506031010	54.8833	55	54.8913	54.8833	0	54.8913	2	2	0	2	1	0	0	52.1919	52.1919	109.054	1	PROCESSED	57604.8728472222	2016-08-04 20:56:54	56385	2013-04-03 00:00:00	56016.6668287037	2012-03-30 16:00:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060080	We propose to observe the very old supernova remnant (SNR) S147 with Suzaku/XIS. S147 has a jet like structure suggesting that it was a core collapse supernova. The formation mechanism of the jet remains unclear for the progenitor which has a small mass and creates a neutron star by its explosion. An asymmetric explosion causes a inhomogeneous metallicity abundance. Therefore, we investigate the inhomogeneous by the plasma diagnosis in the X-ray band to obtain the evidence of the jet formation. This will be the limit of theoretical model for the supernova explosion. S147 is also the GeV gamma-ray source. Therefore, we can study the acceleration mechanism of the cosmic rays in the very old SNR if we detect the nonthermal X-ray emission from it.	GALACTIC DIFFUSE EMISSION	5	C	YOSHITAKA HANABATA		JAP	6	AO6	STUDYING THE SUPERNOVA REMNANT S147 WITH JET STRUCTURE AND GEV GAMMA-RAY EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506031010/	Quick Look
468	VELA PWN E6	131.2685	-45.4809	130.840764	-45.298021	156.629635	-59.743456	264.83769354	-1.61837696	304.5065	55712.9576273148	2011-05-31 22:58:59	55713.2292939815	2011-06-01 05:30:11	506049010	18.1968	15	18.2048	18.1968	0	18.2128	2	2	0	2	1	0	0	14.209	14.209	23.4699	0	PROCESSED	57602.1814699074	2016-08-02 04:21:19	56103	2012-06-25 00:00:00	55735.9387268518	2011-06-23 22:31:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506049010/	Quick Look
469	ERIDANUS_ARCB_SPOT	53.3104	-9.6904	52.708102	-9.857933	48.180187	-27.963294	196.20250346	-48.10218961	67.1761	56138.1083101852	2012-07-30 02:35:58	56139.0792476852	2012-07-31 01:54:07	507032010	40.6186	40	40.6186	40.6186	0	40.6186	2	2	0	2	1	0	0	35.171	35.171	83.8699	1	PROCESSED	57606.7122337963	2016-08-06 17:05:37	56528	2013-08-24 00:00:00	56162.0431018518	2012-08-23 01:02:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070046	We propose Suzaku spectroscopic observations of the Edinanus Super Bubble, the nearest super bubble in our Galaxy. This is a good site to study the density, temperature, metalicity, and ionization status etc. at the rim of super bubbles which might be sources of the Galactic halo or fountains. A series of observations will reveal how the hot plasma is heated and expands as a bubble.	GALACTIC DIFFUSE EMISSION	5	C	NORIKO YAMASAKI		JAP	7	AO7	SUZAKU OBSERVATION OF THE ERIDANUS SUPER BUBBLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507032010/	Quick Look
470	G299.5-0.6	184.8049	-63.1515	184.121711	-62.873858	220.875708	-53.463768	299.30360744	-0.50694599	313.6989	56144.5663773148	2012-08-05 13:35:35	56144.9523032407	2012-08-05 22:51:19	507064010	13.8351	10	13.8431	13.8351	0	13.8431	1	1	0	1	1	0	0	13.2722	13.2722	33.3359	0	PROCESSED	57606.7635763889	2016-08-06 18:19:33	56630	2013-12-04 00:00:00	56264.5463541667	2012-12-03 13:06:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072014	We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed.	GALACTIC DIFFUSE EMISSION	5	A	TOBIAS PRINZ		EUR	7	AO7	IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507064010/	Quick Look
471	G350.1-0.3	260.2697	-37.4549	259.419167	-37.405796	262.032562	-14.282003	350.06545974	-0.33871818	266.4234	55821.2580787037	2011-09-17 06:11:38	55822.9126388889	2011-09-18 21:54:12	506065010	70.1813	70	70.1973	70.1813	0	70.1973	2	2	0	2	1	0	0	60.0704	60.0704	142.9159	0	PROCESSED	57603.2088541667	2016-08-03 05:00:45	55652	2011-04-01 00:00:00	55865.2679282407	2011-10-31 06:25:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506065010/	Quick Look
472	FERMI_BUBBLE_S1	329.068	-46.6182	328.273423	-46.856069	313.852963	-31.76179	351.41726681	-50.59485428	44.0071	56034.6949884259	2012-04-17 16:40:47	56035.2070717593	2012-04-18 04:58:11	507009010	25.3149	20	25.3149	25.3229	0	25.3229	2	2	0	2	1	0	0	24.7973	24.7973	44.2399	0	PROCESSED	57605.1828703704	2016-08-05 04:23:20	56420	2013-05-08 00:00:00	56049.2134722222	2012-05-02 05:07:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507009010/	Quick Look
473	IC 443	94.3026	22.7461	93.545529	22.76515	93.969538	-0.635542	188.89781567	3.10590753	258.9991	56382.4892824074	2013-03-31 11:44:34	56385.8835763889	2013-04-03 21:12:21	507015030	131.1823	300	131.1823	131.1823	0	131.1823	2	2	0	2	1	0	0	113.8514	113.8514	293.2478	1	PROCESSED	57611.0338194444	2016-08-11 00:48:42	56018	2012-04-01 00:00:00	56394.7872337963	2013-04-12 18:53:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070015	The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	7	AO7	DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA --	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015030/	Quick Look
474	G337.2-0.7	249.8782	-47.8314	248.950154	-47.733478	255.175293	-25.419144	337.20769447	-0.7291284	280.8005	56172.5530439815	2012-09-02 13:16:23	56181.2598263889	2012-09-11 06:14:09	507068010	304.1484	300	304.1564	304.1484	0	304.1484	2	2	0	2	1	0	0	275.8448	275.8448	461.2638	9	PROCESSED	57607.2211111111	2016-08-07 05:18:24	56018	2012-04-01 00:00:00	56271.4641203704	2012-12-10 11:08:20	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	7	Ao7	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507068010/	Quick Look
475	CYG_BGD2	306.9576	42.391	306.519882	42.224487	328.379789	58.578032	80.50042704	2.23726855	218.3998	56280.6304166667	2012-12-19 15:07:48	56281.1313888889	2012-12-20 03:09:12	507042010	25.6249	25	25.6249	25.6249	0	25.6489	2	2	0	2	1	0	0	25.025	25.025	43.2739	1	PROCESSED	57608.3181018518	2016-08-08 07:38:04	56683	2014-01-26 00:00:00	56316.5346990741	2013-01-24 12:49:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070060	The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object.	GALACTIC DIFFUSE EMISSION	5	C	TSUNEFUMI MIZUNO		JAP	7	AO7	SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507042010/	Quick Look
476	VELA PWN N5	128.8386	-43.7507	128.405645	-43.5769	151.977516	-59.119722	262.41040878	-1.9318018	327.6005	56110.3470717593	2012-07-02 08:19:47	56110.6620138889	2012-07-02 15:53:18	507052010	18.1486	15	18.1566	18.1486	0	18.1566	2	2	0	2	1	0	0	17.4582	17.4582	27.208	1	PROCESSED	57606.5339930556	2016-08-06 12:48:57	56493	2013-07-20 00:00:00	56127.126712963	2012-07-19 03:02:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070103	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	7	AO7	HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507052010/	Quick Look
477	JUPITER	104.3277	23.0738	103.571845	23.140907	103.162022	0.285142	192.75008442	11.51865374	264.5662	56766.1211111111	2014-04-19 02:54:24	56766.4481365741	2014-04-19 10:45:19	508023080	15.9616	160	15.9776	15.9616	0	15.9806	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57614.9566782407	2016-08-14 22:57:37	57212	2015-07-09 00:00:00	56782.5045486111	2014-05-05 12:06:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023080/	Quick Look
478	GRXE_E_6	268.1913	-26.3855	267.412548	-26.37482	268.368065	-2.954748	3.00107417	-0.0433749	104.9996	56375.3653125	2013-03-24 08:46:03	56377.4119444445	2013-03-26 09:53:12	507073010	101.6745	100	101.6745	101.6745	0	101.6745	2	2	0	2	1	0	0	100.2473	100.2473	176.8078	1	PROCESSED	57610.9396296296	2016-08-10 22:33:04	56018	2012-04-01 00:00:00	56387.5561574074	2013-04-05 13:20:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507073010/	Quick Look
479	JUPITER	103.925	23.1078	103.168762	23.173006	102.79003	0.283016	192.55993514	11.19674467	264.4254	56763.06625	2014-04-16 01:35:24	56763.3890162037	2014-04-16 09:20:11	508023040	14.5693	160	14.5773	14.5693	0	14.5847	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57614.9505902778	2016-08-14 22:48:51	57212	2015-07-09 00:00:00	56839.6932175926	2014-07-01 16:38:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023040/	Quick Look
480	HESS J1534-571 3	234.1055	-57.4189	233.115127	-57.253673	246.756574	-36.836074	323.73309574	-1.36851406	296.0043	56544.6705787037	2013-09-09 16:05:38	56545.1793171296	2013-09-10 04:18:13	508015010	38.7487	40	38.7727	38.7647	0	38.7487	1	1	0	1	1	0	0	29.947	29.947	43.9439	0	PROCESSED	57612.5739814815	2016-08-12 13:46:32	56956	2014-10-26 00:00:00	56588.8303125	2013-10-23 19:55:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080024	Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	8	AO8	RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508015010/	Quick Look
481	HESSJ1858-A	284.5878	2.0823	283.956685	2.013656	286.075284	24.712449	35.57325236	-0.58765875	251.7991	56592.8339467593	2013-10-27 20:00:53	56593.9759027778	2013-10-28 23:25:18	508021010	51.6531	50	51.6611	51.6691	0	51.6531	2	2	0	2	1	0	0	48.7792	48.7792	98.6558	1	PROCESSED	57613.1533796296	2016-08-13 03:40:52	56975	2014-11-14 00:00:00	56608.6801388889	2013-11-12 16:19:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080052	HESS J1858+020 is one of the unidentified TeV objects which are candidates for the origin of the cosmic-ray protons. Recently a supernova remnant G35.6-0.4 and molecular clouds were discovered in the vicinity of HESSJ1858+020. The TeV emission may be generated through the interaction between protons accelerated in the SNR and the molecular clouds. However, a star forming region in the cloud was also discovered by an infrared observation, and the region may be responsible for the acceleration of protons. We propose Suzaku observations of HESSJ1858+020 to clarify what particles are the origin of the TeV emission, and to clarify what accelerates the particles.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	8	AO8	DECISION OF PARTICLE ACCELERATION SOURCE OF HESS J1858+020 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508021010/	Quick Look
482	HESS J1534-571 1	234.0464	-57.1146	233.060336	-56.949151	246.608003	-36.554258	323.88573784	-1.10331415	295.9997	56543.4345138889	2013-09-08 10:25:42	56544.0210300926	2013-09-09 00:30:17	508013010	36.891	40	36.899	36.891	0	36.899	1	1	0	1	1	0	0	36.0704	36.0704	50.6719	0	PROCESSED	57612.5616319444	2016-08-12 13:28:45	56990	2014-11-29 00:00:00	56622.6022569444	2013-11-26 14:27:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080024	Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	8	AO8	RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508013010/	Quick Look
483	SGR C	266.1575	-29.4721	265.359887	-29.451505	266.626891	-6.075935	359.43010365	-0.09543697	265.018	56559.2657060185	2013-09-24 06:22:37	56561.8960763889	2013-09-26 21:30:21	508019010	104.2256	100	104.2495	104.2415	0	104.2256	2	2	0	2	1	0	0	91.1975	91.1975	227.2419	1	PROCESSED	57612.8165277778	2016-08-12 19:35:48	56956	2014-10-26 00:00:00	56588.6596643518	2013-10-23 15:49:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080043	X-ray emissions from giant molecular clouds (X-ray reflection nebula) in the Galactic center region show past activity of the super-massive black hole, Sagittarius (Sgr) A. Using Suzaku, we have found that Sgr A had been in the active phase for almost a thousand years and dropped down to the quiescent level tens of years ago. However, no detailed information during the active phase and transition has been obtained from observations to study a mechanism of the sudden phase change. We aim to observe new information about time variability and relative positions from X-ray reflection nebulae to find the past light curve of Sgr A*. This work will be the grand sum for the Suzaku observation of the Galactic center.	GALACTIC DIFFUSE EMISSION	5	A	MASAYOSHI NOBUKAWA		JAP	8	AO8	PAST HISTORY OF THE SUPER-MASSIVE BLACK HOLE IN THE GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508019010/	Quick Look
484	0509-67.5	77.4163	-67.5163	77.433384	-67.576954	343.17919	-85.012675	278.13367069	-34.57909379	302.8449	56393.0595949074	2013-04-11 01:25:49	56397.1258912037	2013-04-15 03:01:17	508072010	175.9192	320	175.9352	175.9192	0	175.9432	2	2	0	2	1	0	0	166.6668	166.6668	351.2916	3	PROCESSED	57611.1504513889	2016-08-11 03:36:39	56383	2013-04-01 00:00:00	56425.6930439815	2013-05-13 16:37:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081315	We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		USA	8	AO8	LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508072010/	Quick Look
485	MBM16-OFF	46.1075	13.1563	45.420617	12.96209	47.406639	-4.032974	165.8625544	-38.38773927	69.5985	56513.919849537	2013-08-09 22:04:35	56515.9119791667	2013-08-11 21:53:15	508073010	83.0565	80	83.0565	83.0565	0	83.0565	2	2	0	2	1	0	0	81.1386	81.1386	172.0979	2	PROCESSED	57612.2143981482	2016-08-12 05:08:44	56953	2014-10-23 00:00:00	56587.5588541667	2013-10-22 13:24:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081322	We propose the observation of three off-cloud targets near the targets of the Solar Wind Charge Exchange (SWCX) Key Project to study the properties of the Diffuse X-ray Background below 1 keV, with particular focus on the characterization of the Galactic Halo. The Key Project targets are at a distance of a few hundreds pc from the Sun and their high density portions shields about 90% of X-rays at the O VII energy, our proposed targets, instead, shield only about 50% of the Galactic Halo emission. The contrast between on- and off-cloud allows us to disentangle the foreground and background emissions. In particular we will focus on the properties of the galactic halo, which dominates the oxygen background emission.	GALACTIC DIFFUSE EMISSION	5	A	EUGENIO URSINO		USA	8	AO8	PROPERTIES OF THE GALACTIC HALO THROUGH SHADOW OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508073010/	Quick Look
486	GRXE_E_8	268.4708	-25.9492	267.69465	-25.939883	268.614118	-2.515578	3.50431952	-0.037979	86.7223	56718.7089236111	2014-03-02 17:00:51	56720.9585069445	2014-03-04 23:00:15	508077010	103.132	100	103.14	103.132	0	103.14	2	2	0	2	1	0	0	94.8538	94.8538	194.3449	2	PROCESSED	57613.971712963	2016-08-13 23:19:16	56383	2013-04-01 00:00:00	56775.6980787037	2014-04-28 16:45:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086001	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	8	AO8	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508077010/	Quick Look
487	VELA PWN GEV2	128.4409	-44.9066	128.017684	-44.734295	152.61498	-60.265788	263.16834954	-2.85026128	119.7193	56985.851099537	2014-11-24 20:25:35	56986.5001273148	2014-11-25 12:00:11	509012010	19.1078	15	19.1398	19.1238	0	19.1078	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.8168981482	2016-08-16 19:36:20	57366	2015-12-10 00:00:00	57009.4112268518	2014-12-18 09:52:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090046	We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	9	AO9	X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509012010/	Quick Look
488	HESS J1641-463	250.2616	-46.3013	249.347836	-46.205158	255.208281	-23.867274	338.52580532	0.09066192	282.4572	56900.1342939815	2014-08-31 03:13:23	56902.1166435185	2014-09-02 02:47:58	509010020	0	40	0	0	0	0	0	0	0	0	0	0	0	0	0	0	0	PROCESSED	57616.5303356482	2016-08-16 12:43:41	56748	2014-04-01 00:00:00	57122.3887268518	2015-04-10 09:19:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090045	The origin of cosmic rays has been one of the biggest problems in modern astrophysics. TeV gamma-ray observations provide indirect evidences of cosmic ray acceleration, although the sources detected so far have softer spectra than what would be expected by particle accelerators to explain the observed distribution of cosmic rays at the knee. HESS J1641-463 is the hardest TeV gamma-ray source ever found. With Suzaku's large effective area, and low and stable background, we will perform the first deep X-ray observation of this source to seek for its X-ray counterpart, and to identify its nature. It will provide a direct look into the physics of the highest energy particle accelerators in our Galaxy, responsible for the cosmic ray spectrum up to the spectral knee at PeV energies.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	9	AO9	IDENTIFYING THE X-RAY COUNTERPART OF THE HARDEST SOURCE HUMAN EVER DETECTED	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509010020/	Quick Look
489	CIZA J1358.9-4750_SE	209.9655	-47.9267	209.17324	-47.684492	226.050091	-33.219593	314.62109256	13.3860264	293	56881.8273032407	2014-08-12 19:51:19	56882.7188773148	2014-08-13 17:15:11	509026010	41.3601	40	41.3601	41.3601	0	41.3601	2	2	0	2	1	0	0	5.8509	5.8509	14.04	0	PROCESSED	57616.4947800926	2016-08-16 11:52:29	57270	2015-09-05 00:00:00	56902.1901273148	2014-09-02 04:33:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090102	Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS.	GALACTIC DIFFUSE EMISSION	5	B	YUICHI KATO		JAP	9	AO9	OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509026010/	Quick Look
490	G93.3+6.9 NW RIM	312.9527	55.5354	312.608547	55.346344	352.30712	67.106977	93.368132	7.08938459	52.0991	56814.8070023148	2014-06-06 19:22:05	56817.24125	2014-06-09 05:47:24	509040010	107.8986	100	107.9066	107.9066	0	107.8986	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.2100115741	2016-08-15 05:02:25	57236	2015-08-02 00:00:00	56869.6106481482	2014-07-31 14:39:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091316	We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN.	GALACTIC DIFFUSE EMISSION	5	C	MICHAEL STAGE		USA	9	AO9	G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509040010/	Quick Look
491	OFF-FIELD4	173.7625	-36.8508	173.145535	-36.574162	191.286304	-35.787139	286.33839516	23.54732297	109.4045	57008.1600925926	2014-12-17 03:50:32	57009.6814699074	2014-12-18 16:21:19	509045010	81.321	80	81.321	81.321	0	81.321	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.5308680556	2016-08-17 12:44:27	56748	2014-04-01 00:00:00	57112.4059490741	2015-03-31 09:44:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091321	Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma.	GALACTIC DIFFUSE EMISSION	5	C	ANJALI GUPTA		USA	9	AO9	CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509045010/	Quick Look
492	FERMI_JET_COCOON_5	306.4609	-33.261	305.672059	-33.424933	300.742491	-13.631284	9.28791468	-33.23258901	260.3818	56968.8506481482	2014-11-07 20:24:56	56969.3612847222	2014-11-08 08:40:15	509051010	22.0438	20	22.0518	22.0438	0	22.0573	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7478125	2016-08-16 17:56:51	57358	2015-12-02 00:00:00	56982.4350694445	2014-11-21 10:26:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091322	The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way.	GALACTIC DIFFUSE EMISSION	5	C	MATTHEW MILLER		USA	9	AO9	OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509051010/	Quick Look
493	3C400.2 SW	294.5545	17.147	293.991762	17.032549	300.267467	38.043132	53.47817432	-2.17482828	81.5886	56761.5284375	2014-04-14 12:40:57	56762.0730555556	2014-04-15 01:45:12	509069010	24.1528	20	24.1528	24.1528	0	24.1537	2	2	0	2	1	0	0	23.915	23.915	47.0479	3	PROCESSED	57614.2434027778	2016-08-14 05:50:30	57138	2015-04-26 00:00:00	56772.6111226852	2014-04-25 14:40:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092010	Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances.	GALACTIC DIFFUSE EMISSION	5	A	JACCO VINK		EUR	9	AO9	THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509069010/	Quick Look
494	GB_NORTH_2	265.5401	-28.4005	264.749404	-28.376931	266.05313	-5.020438	0.05846164	0.92703829	108.0199	57106.6765856482	2015-03-25 16:14:17	57108.7243634259	2015-03-27 17:23:05	509078010	95.3893	100	95.3893	99.8284	0	99.8124	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8717361111	2016-08-17 20:55:18	56748	2014-04-01 00:00:00	57119.4143981482	2015-04-07 09:56:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096002	The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	9	AO9	MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY-	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509078010/	Quick Look
495	GB_NORTH_3	265.8335	-28.3716	265.042917	-28.349452	266.311245	-4.983802	0.21886292	0.72273612	108.0564	57108.7249074074	2015-03-27 17:23:52	57110.9703703704	2015-03-29 23:17:20	509079010	106.9674	100	106.9674	108.1889	0	108.1889	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8792939815	2016-08-17 21:06:11	56748	2014-04-01 00:00:00	57119.4192708333	2015-04-07 10:03:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096002	The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	9	AO9	MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY-	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509079010/	Quick Look
496	SN1006_BGD4	226.2633	-42.7499	225.438524	-42.555935	236.137627	-24.311137	327.5160888	13.6541367	286.3809	56889.2090740741	2014-08-20 05:01:04	56889.7793865741	2014-08-20 18:42:19	509086010	33.5116	30	33.5156	33.5116	0	33.5196	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5076851852	2016-08-16 12:11:04	56748	2014-04-01 00:00:00	56910.6440162037	2014-09-10 15:27:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096004	We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		USA	9	AO9	THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509086010/	Quick Look
497	RXJ1713-3946	258.5527	-40.0289	257.68331	-39.971559	260.849002	-16.950052	347.19063141	-0.73133412	268.0015	53997.9147569444	2006-09-19 21:57:15	53998.4425925926	2006-09-20 10:37:20	501070010	20.7442	20	20.7442	20.7522	20.7522	20.7522	2	2	2	2	1	0	0	22.0266	22.0266	45.5959	1	PROCESSED	57535.6347685185	2016-05-27 15:14:04	54526	2008-03-01 00:00:00	54021.1763541667	2006-10-13 04:13:57	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501070010/	Quick Look
498	GALACTIC CENTER GC10	266.4308	-29.5343	265.632731	-29.515028	266.867639	-6.131965	359.50116476	-0.33080245	109.7996	54171.9994097222	2007-03-12 23:59:09	54172.6529976852	2007-03-13 15:40:19	501055010	27.2257	25	27.2257	27.2497	0	27.2337	2	2	0	2	1	0	0	21.1819	21.1819	56.4539	0	PROCESSED	57537.6665740741	2016-05-29 15:59:52	54736	2008-09-27 00:00:00	54182.3161342593	2007-03-23 07:35:14	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501055010/	Quick Look
499	COMET_8P_TUTTLE-P2_11	40.2448	-37.071	39.739892	-37.284352	20.945205	-49.302594	243.11250517	-64.87732742	253.5002	54491.3630439815	2008-01-26 08:42:47	54491.4959953704	2008-01-26 11:54:14	502063110	6.3822	6.7	6.3902	6.3822	0	6.3902	1	1	0	1	1	0	0	6.8385	6.8385	11.4799	0	PROCESSED	57541.406712963	2016-06-02 09:45:40	54912	2009-03-22 00:00:00	54546.1994097222	2008-03-21 04:47:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063110/	Quick Look
500	RXJ1713-3946_ID2	258.3083	-40.2394	257.437413	-40.180894	260.672603	-17.175399	346.91054647	-0.70324775	87.0013	55243.7284722222	2010-02-16 17:29:00	55244.1258564815	2010-02-17 03:01:14	504028010	19.0093	20	19.0093	19.0173	0	19.0173	2	2	0	2	1	0	0	11.8263	11.8263	34.3319	0	PROCESSED	57550.6004976852	2016-06-11 14:24:43	55622	2011-03-02 00:00:00	55256.0518171296	2010-03-01 01:14:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040021	We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009.	GALACTIC DIFFUSE EMISSION	5	B	TADAYUKI TAKAHASHI		JAP	4	AO4	STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504028010/	Quick Look
501	CTB109 NORTHEAST	345.764	59.0015	345.238644	58.732029	24.240732	56.810585	109.36320905	-0.98507066	252.0025	55910.0815393518	2011-12-15 01:57:25	55910.7522106482	2011-12-15 18:03:11	506039010	30.4058	30	30.4058	30.4058	0	30.4058	2	2	0	2	1	0	0	30.7473	30.7473	57.9219	1	PROCESSED	57604.1437268518	2016-08-04 03:26:58	56289	2012-12-28 00:00:00	55921.9865277778	2011-12-26 23:40:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060100	Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations.	GALACTIC DIFFUSE EMISSION	5	C	TOSHIO NAKANO		JAP	6	AO6	SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506039010/	Quick Look
502	GALACTIC CENTER GC9	266.6299	-29.2499	265.833607	-29.231598	267.035089	-5.843458	359.83430056	-0.33104727	109.8001	54171.3410532407	2007-03-12 08:11:07	54171.9988888889	2007-03-12 23:58:24	501054010	26.1044	25	26.1044	26.1044	0	26.1044	2	2	0	2	1	0	0	23.5424	23.5424	56.8299	0	PROCESSED	57537.6542013889	2016-05-29 15:42:03	54736	2008-09-27 00:00:00	54182.2954166667	2007-03-23 07:05:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501054010/	Quick Look
503	VERJ2019_P3	304.792	36.828	304.322431	36.670095	321.385407	54.239801	74.98489793	0.41476969	250.4389	56971.0428009259	2014-11-10 01:01:38	56972.0349537037	2014-11-11 00:50:20	509030010	41.0715	40	41.0795	41.0715	0	41.0875	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7632175926	2016-08-16 18:19:02	57352	2015-11-26 00:00:00	56982.4314467593	2014-11-21 10:21:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090120	The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at elongated TeV gamma-ray emission found by Milagro and recently resolved by VERITAS. Although an energetic pulsar PSR J2021+3651 coincides with one of TeV peaks, most of gamma-ray emission still remains unexplained. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we aim to detect X-ray counterparts, presumably unknown pulsar wind nebulae. Connection with a Wolf-Rayet star and an HII region inside this region, which positionally coincide with the gamma-ray peak, will also be investigated.	GALACTIC DIFFUSE EMISSION	5	C	TSUNEFUMI MIZUNO		JAP	9	AO9	SEARCH FOR TEV ACCELERATORS IN NEARBY STAR-FORMING REGION CYGNUS-X WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509030010/	Quick Look
504	VELA PWN NE3	131.0442	-44.0836	130.607036	-43.901563	154.967747	-58.624056	263.64329985	-0.87547181	123.9937	55895.188900463	2011-11-30 04:32:01	55895.621724537	2011-11-30 14:55:17	506043010	17.7999	15	17.8066	17.7999	0	17.8066	2	2	0	2	1	0	0	13.012	13.012	37.3959	0	PROCESSED	57604.0129050926	2016-08-04 00:18:35	56274	2012-12-13 00:00:00	55907.1603703704	2011-12-12 03:50:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	C	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506043010/	Quick Look
505	VELA PWN E1	129.1398	-45.2732	128.71724	-45.098238	153.84788	-60.334335	263.75797839	-2.67419196	142.334	55916.0561226852	2011-12-21 01:20:49	55916.622337963	2011-12-21 14:56:10	506044010	17.718	15	17.718	17.718	0	17.718	2	2	0	2	1	0	0	16.6284	16.6284	48.8959	0	PROCESSED	57604.1814814815	2016-08-04 04:21:20	56305	2013-01-13 00:00:00	55937.7696527778	2012-01-11 18:28:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	C	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506044010/	Quick Look
506	HB9-WEST	74.7057	46.2322	73.785793	46.156635	78.534376	23.399217	160.54700874	2.22396757	74.7402	56930.7930671296	2014-09-30 19:02:01	56931.9168518518	2014-10-01 22:00:16	509032010	49.7688	50	49.7688	49.7688	0	49.7688	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.5952662037	2016-08-16 14:17:11	57345	2015-11-19 00:00:00	56979.4048611111	2014-11-18 09:43:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091312	We propose to conduct two pointed observations of the Galactic supernova remnant (SNR) HB9 (G160.9+2.6) with Suzaku. HB9 is a member of the class of Galactic SNRs which are distinguished by their contrasting radio and X-ray morphologies. Prior X-ray observations of HB9 have suggested that the SNR may have a hard component to its X-ray emission, but the true nature of this emission and its origin (a background AGN, intercluster gas associated with the cluster that harbors the AGN or the SNR itself) remains elusive. Our proposed observations will help identify the true nature of the hard emission as well as search for spectral variations (and possible overionization) in the properties of the X-ray emitting plasma associated with the SNR.	GALACTIC DIFFUSE EMISSION	5	A	THOMAS PANNUTI		USA	9	AO9	SUZAKU OBSERVATIONS OF THE GALACTIC SUPERNOVA REMNANT HB9 (G160.9+2.6)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509032010/	Quick Look
507	WESTERLUND1_3	252.0931	-46.1953	251.177246	-46.107555	256.5618	-23.584825	339.43313351	-0.79934014	282.1087	55462.25625	2010-09-23 06:09:00	55463.3946296296	2010-09-24 09:28:16	505051010	50.2046	50	50.2046	50.2046	0	50.2046	2	2	0	2	1	0	0	40.7966	40.7966	98.3438	1	PROCESSED	57553.5465162037	2016-06-14 13:06:59	55840	2011-10-06 00:00:00	55474.0771180556	2010-10-05 01:51:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050078	TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster.	GALACTIC DIFFUSE EMISSION	5	A	HIRONORI MATSUMOTO		JAP	5	AO5	IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505051010/	Quick Look
508	LDN1563	75.5225	13.8674	74.815655	13.796139	75.781481	-8.861998	187.1486738	-16.70848186	83.2339	56902.1301041667	2014-09-02 03:07:21	56904.0071643518	2014-09-04 00:10:19	509075010	41.1155	80	41.1396	41.1395	0	41.1155	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5646296296	2016-08-16 13:33:04	56748	2014-04-01 00:00:00	56926.5705439815	2014-09-26 13:41:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096001	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	9	AO9	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509075010/	Quick Look
509	73P/SW3	18.1606	-9.2654	17.534064	-9.530431	13.093401	-15.671197	139.58635244	-71.44823165	59.3999	53894.1358333333	2006-06-08 03:15:36	53894.2085416667	2006-06-08 05:00:18	500014080	1.8637	35	1.8637	1.8637	1.8637	1.8637	2	2	2	2	1	0	0	1.9212	1.9212	6.2779	0	PROCESSED	57534.5937731482	2016-05-26 14:15:02	54267	2007-06-16 00:00:00	54052.5243171296	2006-11-13 12:35:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014080/	Quick Look
510	SN1006_BGD1	225.9444	-42.5002	225.122216	-42.305131	235.809577	-24.144105	327.43636425	13.98792654	286.4314	56887.5218171296	2014-08-18 12:31:25	56888.0141203704	2014-08-19 00:20:20	509083010	32.1009	30	32.1089	32.1089	0	32.1009	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.5011111111	2016-08-16 12:01:36	56748	2014-04-01 00:00:00	56910.6401736111	2014-09-10 15:21:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096004	We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		USA	9	AO9	THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509083010/	Quick Look
511	73P/SW3	18.3869	-9.3535	17.760674	-9.618192	13.270909	-15.839893	140.33698221	-71.47421859	59.3991	53894.4684490741	2006-06-08 11:14:34	53894.5356365741	2006-06-08 12:51:19	500014130	1.6939	35	1.6939	1.6939	1.6939	1.6939	1	1	1	1	1	0	0	1.694	1.694	5.804	0	PROCESSED	57534.6023611111	2016-05-26 14:27:24	54267	2007-06-16 00:00:00	54052.5234722222	2006-11-13 12:33:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014130/	Quick Look
512	ASO0147	98.4346	6.5402	97.762331	6.579413	98.750752	-16.644923	205.09585789	-0.932863	292.0552	54931.9181481482	2009-04-10 22:02:08	54932.5036921296	2009-04-11 12:05:19	504047010	24.0413	20	24.0413	24.0413	0	24.0413	2	2	0	2	1	0	0	23.2409	23.2409	50.562	1	PROCESSED	57546.1122685185	2016-06-07 02:41:40	55324	2010-05-08 00:00:00	54949.5271180556	2009-04-28 12:39:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 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 DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504047010/	Quick Look
513	G25.5+0.0	279.4506	-6.6057	278.777895	-6.649808	279.78518	16.514382	25.50196825	0.00652115	74.2354	54927.1234490741	2009-04-06 02:57:46	54928.7446064815	2009-04-07 17:52:14	504099010	52.7375	50	52.7375	52.7375	0	52.7375	2	2	0	2	1	0	0	44.5703	44.5703	140.042	3	PROCESSED	57546.0819675926	2016-06-07 01:58:02	54922	2009-04-01 00:00:00	54949.4845023148	2009-04-28 11:37:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504099010/	Quick Look
514	SN1006_BGD2	226.2226	-42.2202	225.40133	-42.0261	235.931519	-23.815123	327.76465581	14.12663913	286.4366	56888.0146875	2014-08-19 00:21:09	56888.6460416667	2014-08-19 15:30:18	509084010	34.8497	30	34.8793	34.8817	0	34.8497	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5054050926	2016-08-16 12:07:47	56748	2014-04-01 00:00:00	56910.6406365741	2014-09-10 15:22:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096004	We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		USA	9	AO9	THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509084010/	Quick Look
515	M17	275.2076	-16.1829	274.486266	-16.206429	275.030512	7.16685	15.0906551	-0.7606192	110.1996	53805.8263425926	2006-03-11 19:49:56	53808.5349421296	2006-03-14 12:50:19	501003010	102.7021	100	102.7101	102.7101	102.7021	102.7101	2	2	2	2	1	0	0	92.5661	92.5661	233.9678	4	PROCESSED	57533.2492939815	2016-05-25 05:58:59	54394	2007-10-21 00:00:00	53905.822662037	2006-06-19 19:44:38	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010066	Recent Chandra observations discovered that HII regions possess a few MK extended plasma, but the origin of the emission is still unknown. We propose to observe M17, which has the most spectacular sample of such emission. A superb soft-band response of XIS will enable us to measure the strengths of O and N emission lines, giving us strong arguments to elucidate the cause of the emission. A 300 ks Chandra observation is planned this year in addition to the existing 40 ks data, which will help us to discriminate the point source contribution.	GALACTIC DIFFUSE EMISSION	5	A	MASAHIRO TSUJIMOTO		JAP	1	AO1	XIS INVESTIGATION FOR THE ORIGIN OF DIFFUSE X-RAY EMISSION IN GALACTIC H II REGIONS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501003010/	Quick Look
516	CTB 37B	258.4918	-38.2006	257.636889	-38.143005	260.643359	-15.13191	348.64561092	0.37683278	270.1267	53974.0604976852	2006-08-27 01:27:07	53976.2398032407	2006-08-29 05:45:19	501007010	82.8151	80	82.8711	82.8151	82.8791	82.8631	2	2	2	2	1	0	0	68.8603	68.8603	188.2779	2	PROCESSED	57535.4428703704	2016-05-27 10:37:44	54526	2008-03-01 00:00:00	54053.4840162037	2006-11-14 11:36:59	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010042	The Galactic Plane Survey with HESS found several new TeV sources, called as "dark particle accelerators". They must be powerful cosmic-ray accelerators, although their origin is still unknown due to the lack of information in other wavelengths. We investigate one of the extended sample with radio SNR counterpart, CTB 37B, which is marginally detected on the edge of ASCA GIS. ASCA spectrum shows rather soft power-law feature, indicating that there are both thermal and non-thermal X-ray emission. With the low background of XISs and HXD, parameters of both components are determined with 80 ks exposure. The non-thermal component suggests the new sample of accelerators, and the thermal compopent reveals the condition of the proton acceleration site, for the first time.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	1	AO1	UNCOVERING THE NATURE OF DARK PARTICLE ACCELERATORS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501007010/	Quick Look
517	(L,B)=(0.25,-0.27)	266.8068	-28.8823	266.012807	-28.864862	267.181973	-5.472426	0.22878525	-0.27253682	265.3343	54343.5232986111	2007-08-31 12:33:33	54346.7919560185	2007-09-03 19:00:25	502022010	134.7904	133	134.7984	134.8064	0	134.7904	2	2	0	2	1	0	0	116.8425	116.8425	282.3759	1	PROCESSED	57539.9810185185	2016-05-31 23:32:40	54724	2008-09-15 00:00:00	54356.5238657407	2007-09-13 12:34:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020044	The Suzaku PV observations found that the diffuse X-rays (6.7 and 6.9 keV-lines) from the GC region can well be explained by a thermal emission from hot plasma with kT=6-7keV (GCDX). The comparison of Suzaku and VLA 90cm images show a hit for special correlation, suggest a magnetic confinement of GCDX. Thus, in order to search for new SNRs and investigate the galactic latitude dependency of the GCDX, we make a GC observation with the aiming point of (l,b)=(0.25, -0.27). We also see the correlation of GCDX with the radio.	GALACTIC DIFFUSE EMISSION	5	B	TAKESHI TSURU		JAP	2	AO2	GLOBAL STRUCTURES OF THE GALACTIC CENTER DIFFUSE X-RAY PLASMA (GCDX)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502022010/	Quick Look
518	GC16	267.4868	-29.3131	266.689954	-29.298954	267.787562	-5.891312	0.16607902	-1.00376926	260.5335	54383.6397800926	2007-10-10 15:21:17	54384.0419444444	2007-10-11 01:00:24	502004010	19.873	20	19.873	19.8903	0	19.8743	1	1	0	1	1	0	0	18.8321	18.8321	34.736	0	PROCESSED	57540.2356597222	2016-06-01 05:39:21	54771	2008-11-01 00:00:00	54402.5680208333	2007-10-29 13:37:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502004010/	Quick Look
519	GALACTIC CENTER GC11	266.231	-29.8182	265.431151	-29.797955	266.700372	-6.420209	359.16839231	-0.33075371	109.7993	54172.6536111111	2007-03-13 15:41:12	54173.2086111111	2007-03-14 05:00:24	501056010	26.5374	25	26.5454	26.5454	0	26.5374	2	2	0	2	1	0	0	25.2789	25.2789	47.946	0	PROCESSED	57537.6702199074	2016-05-29 16:05:07	54736	2008-09-27 00:00:00	54182.3328125	2007-03-23 07:59:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501056010/	Quick Look
520	COMET_8P_TUTTLE-P2_17	40.6015	-37.8518	40.101512	-38.064027	20.766573	-50.125126	244.68288405	-64.39021906	254.0645	54492.1630439815	2008-01-27 03:54:47	54492.2959953704	2008-01-27 07:06:14	502063170	5.1495	5	5.1495	5.1495	0	5.1495	1	1	0	1	1	0	0	5.4142	5.4142	11.432	0	PROCESSED	57541.4188425926	2016-06-02 10:03:08	54912	2009-03-22 00:00:00	54546.2465509259	2008-03-21 05:55:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063170/	Quick Look
521	HESS J1841-55 1	279.8307	-5.8897	279.161498	-5.93564	280.231092	17.202355	26.31151486	-0.00077944	87.7391	55645.2916782407	2011-03-25 07:00:01	55646.4446180556	2011-03-26 10:40:15	505088010	49.652	50	49.652	49.652	0	49.652	2	2	0	2	1	0	0	39.8604	39.8604	99.5978	0	PROCESSED	57601.3329976852	2016-08-01 07:59:31	55287	2010-04-01 00:00:00	55658.1566087963	2011-04-07 03:45:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505088010/	Quick Look
522	GC_LARGEPROJECT7	265.6744	-30.0704	264.873054	-30.047455	266.222278	-6.685926	358.7007591	-0.05229538	265.9998	54725.0356365741	2008-09-16 00:51:19	54727.1975	2008-09-18 04:44:24	503013010	104.769	100	104.777	104.777	0	104.769	2	2	0	2	1	0	0	93.9013	93.9013	186.7098	3	PROCESSED	57543.8883564815	2016-06-04 21:19:14	54557	2008-04-01 00:00:00	54780.5885532407	2008-11-10 14:07:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503013010/	Quick Look
523	RXJ_0852-4622_NW_offset	135.1284	-47.9102	134.705364	-47.713589	163.727844	-60.335158	268.39892579	-1.13950817	140.267	53727.3040393518	2005-12-23 07:17:49	53728.368912037	2005-12-24 08:51:14	500010020	59.1784	50	59.1784	59.1925	59.2026	59.1925	2	2	2	2	1	0	0	63.4821	63.4821	91.9959	0	PROCESSED	57532.4967708333	2016-05-24 11:55:21	54247	2007-05-27 00:00:00	54039.2486226852	2006-10-31 05:58:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001048	We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		JAP	0	SWG	HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500010020/	Quick Look
524	VELA JR P4	132.5157	-45.5453	132.084337	-45.3579	158.164513	-59.340232	265.43667302	-0.97855833	347.0031	54286.1062847222	2007-07-05 02:33:03	54286.4480787037	2007-07-05 10:45:14	502026010	10.9724	10	10.9724	10.9724	0	10.9724	2	2	0	2	1	0	0	11.2959	11.2959	29.5119	1	PROCESSED	57539.0994791667	2016-05-31 02:23:15	54759	2008-10-20 00:00:00	54328.4405787037	2007-08-16 10:34:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502026010/	Quick Look
525	GC_LARGEPROJECT12	264.5602	-31.5978	263.749148	-31.569439	265.310572	-8.245043	356.8985011	-0.05173107	288.0843	54733.394375	2008-09-24 09:27:54	54733.9377777778	2008-09-24 22:30:24	503018010	29.4012	50	29.4125	29.4125	0	29.4012	2	2	0	2	1	0	0	26.6716	26.6716	46.942	0	PROCESSED	57543.9951851852	2016-06-04 23:53:04	54557	2008-04-01 00:00:00	54780.4814583333	2008-11-10 11:33:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503018010/	Quick Look
526	GC_LARGEPROJECT14	264.2413	-32.0163	263.427554	-31.98639	265.053396	-8.67384	356.39993487	-0.04727305	95.7088	54883.0527199074	2009-02-21 01:15:55	54884.7911342593	2009-02-22 18:59:14	503020010	61.0441	50	61.0681	61.0441	0	61.0601	2	2	0	2	1	0	0	51.7185	51.7185	150.1319	1	PROCESSED	57545.6307175926	2016-06-06 15:08:14	54557	2008-04-01 00:00:00	54895.6029166667	2009-03-05 14:28:12	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503020010/	Quick Look
527	VELA JR P21	133.1972	-46.3295	132.769289	-46.139656	159.781258	-59.750169	266.34323773	-1.11269222	347.0005	54651.5833680556	2008-07-04 14:00:03	54652.0557175926	2008-07-05 01:20:14	503033010	14.2872	10	14.2952	14.2872	0	14.3032	2	2	0	2	1	0	0	12.0665	12.0665	40.8019	1	PROCESSED	57542.9629398148	2016-06-03 23:06:38	55036	2009-07-24 00:00:00	54665.3234375	2008-07-18 07:45:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503033010/	Quick Look
528	VELA JR P36	133.0606	-47.2239	132.639922	-47.034529	160.606122	-60.550234	266.97132611	-1.75647675	346.9998	54656.5145833333	2008-07-09 12:21:00	54656.9168634259	2008-07-09 22:00:17	503048010	11.1226	10	11.1306	11.1226	0	11.1386	2	2	0	2	1	0	0	9.3838	9.3838	34.7499	1	PROCESSED	57543.0132175926	2016-06-04 00:19:02	55037	2009-07-25 00:00:00	54670.2692361111	2008-07-23 06:27:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503048010/	Quick Look
529	CYGNUS LOOP (P23)	312.4772	32.3587	311.966597	32.171629	327.828669	47.6396	75.1675214	-7.32455162	61.8892	54620.7530439815	2008-06-03 18:04:23	54621.1473842593	2008-06-04 03:32:14	503059010	19.457	15	19.457	19.457	0	19.457	1	1	0	1	1	0	0	17.2771	17.2771	34.0639	0	PROCESSED	57542.7106944444	2016-06-03 17:03:24	55003	2009-06-21 00:00:00	54636.2328240741	2008-06-19 05:35:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503059010/	Quick Look
530	CYGNUS LOOP (P28)	313.4797	29.8934	312.955126	29.702774	327.568716	45.03529	73.77252886	-9.54040793	49.1005	54600.0501273148	2008-05-14 01:12:11	54600.5334953704	2008-05-14 12:48:14	503064010	18.1693	15	18.1773	18.1853	0	18.1693	2	2	0	2	1	0	0	16.443	16.443	41.756	0	PROCESSED	57542.5291898148	2016-06-03 12:42:02	54975	2009-05-24 00:00:00	54609.1904282407	2008-05-23 04:34:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503064010/	Quick Look
531	G18.0-0.7	276.56	-13.5781	275.85231	-13.608204	276.459314	9.715522	18.00442084	-0.69482715	92.0001	54909.8982060185	2009-03-19 21:33:25	54911.080775463	2009-03-21 01:56:19	503086010	52.0592	50	52.0592	52.0672	0	52.0672	2	2	0	2	1	0	0	46.3036	46.3036	102.1458	2	PROCESSED	57547.7369560185	2016-06-08 17:41:13	55329	2010-05-13 00:00:00	54923.3684490741	2009-04-02 08:50:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031203	By studying pulsar wind nebulae, the synchrotron nebulae powered by a neutron star's loss of rotational energy, it is possible to determine the energetics of both the progenitor supernova and central neutron star. This requires estimates of the expansion velocity and mass swept-up the pulsar wind nebulae, best obtained by analyzing the spectrum of the thermal X-rays emitting by this material. In the proposal, we request a 50ks observation of four of the most energetic pulsar wind nebulae in the Milky Way to both detect such thermal X-ray emission and use the measured spectral properties to infer the ejecta mass and kinetic energy of their progenitor supernova and the initial spin period of the central neutron star -- all currently unmeasurable using the currently available information.	GALACTIC DIFFUSE EMISSION	5	C	JOSEPH GELFAND		USA	3	AO3	STUDYING THE PROGENITOR SUPERNOVA AND CENTRAL NEUTRON STAR OF PULSAR WIND NEBULAE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503086010/	Quick Look
532	GALACTIC_BULGE12	270.5539	-32.7559	269.734001	-32.756597	270.462385	-9.315774	358.50046577	-5.00243267	271.4834	55119.6475462963	2009-10-15 15:32:28	55120.7502199074	2009-10-16 18:00:19	504095010	48.2622	50	48.2622	48.2622	0	48.2622	3	2	0	2	1	0	0	38.358	38.358	95.2619	1	PROCESSED	57548.9040856482	2016-06-09 21:41:53	54922	2009-04-01 00:00:00	55133.2742824074	2009-10-29 06:34:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504095010/	Quick Look
533	GC SGR D NORTH	266.9758	-27.7178	266.189062	-27.7012	267.305981	-4.305004	1.30220378	0.20283685	108.7992	54173.2100578704	2007-03-14 05:02:29	54174.7883564815	2007-03-15 18:55:14	501058010	63.2422	63	63.2502	63.2422	0	63.2582	2	2	0	2	1	0	0	51.1479	51.1479	136.3519	0	PROCESSED	57537.7302546296	2016-05-29 17:31:34	54735	2008-09-26 00:00:00	54182.440462963	2007-03-23 10:34:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501058010/	Quick Look
534	HESS J1718-385	259.5578	-38.4584	258.700067	-38.405877	261.528277	-15.323293	348.92137939	-0.45364037	266.9006	54706.233599537	2008-08-28 05:36:23	54706.9286342593	2008-08-28 22:17:14	503108010	23.5097	20	23.5097	23.5097	0	23.5097	2	2	0	2	1	0	0	19.4402	19.4402	60.0479	1	PROCESSED	57543.4301851852	2016-06-04 10:19:28	55093	2009-09-19 00:00:00	54720.4386689815	2008-09-11 10:31:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032026	HESS J1718-385 is a newly discovered Very High Energy (VHE) source with an unusually hard energy spectrum, close to an energetic pulsar. The classification as a VHE Pulsar Wind Nebula (PWN) was confirmed by observations of the region with XMM-Newton and Suzaku. XMM showed a compact X-ray PWN around the pulsar, whereas Suzaku revealed low surface brightness emission close to the VHE source. To morphologically connect this low surface brightness emission to the X-ray PWN, we propose another short, 20 ksec Suzaku pointing, aiming between the VHE source center and the pulsar location. The data will allow to identify the new Suzaku source with the compact X-ray PWN. The spectra will be used to investigate the unusual particle energy distribution that is derived from the hard VHE spectrum.	GALACTIC DIFFUSE EMISSION	5	A	GERD PUEHLHOFER		EUR	3	AO3	SUZAKU OBSERVATIONS OF THE LOW SURFACE BRIGHTNESS X-RAY PULSAR WIND NEBULA CANDIDATE ASSOCIATED WITH HESS J1718-385	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503108010/	Quick Look
535	ASO0431	286.9632	6.0295	286.350421	5.949691	289.23811	28.344266	40.16756672	-0.88470452	90.0004	54936.153287037	2009-04-15 03:40:44	54936.8141666667	2009-04-15 19:32:24	504043010	24.5222	20	24.5222	24.5222	0	24.5222	2	2	0	2	1	0	0	18.105	18.105	57.0739	0	PROCESSED	57546.1491087963	2016-06-07 03:34:43	55324	2010-05-08 00:00:00	54949.5652777778	2009-04-28 13:34:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 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 DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504043010/	Quick Look
536	RXJ1713-3946	257.9704	-39.5791	257.105134	-39.519003	260.343852	-16.539668	347.29183097	-0.10508063	267.9995	53989.172025463	2006-09-11 04:07:43	53989.5306365741	2006-09-11 12:44:07	501063010	18.422	20	18.422	18.422	18.422	18.422	2	2	2	2	1	0	0	17.7597	17.7597	30.9719	1	PROCESSED	57535.5249537037	2016-05-27 12:35:56	54526	2008-03-01 00:00:00	54021.1086458333	2006-10-13 02:36:27	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501063010/	Quick Look
537	RIM5	311.5286	30.6813	311.011535	30.497677	325.775502	46.411023	73.33464134	-7.73161485	255.8951	55155.3611689815	2009-11-20 08:40:05	55155.7953356482	2009-11-20 19:05:17	504009010	15.8502	15	15.8502	15.8502	0	15.8502	2	2	0	2	1	0	0	12.2891	12.2891	37.5039	0	PROCESSED	57549.4934259259	2016-06-10 11:50:32	55534	2010-12-04 00:00:00	55166.4265277778	2009-12-01 10:14:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504009010/	Quick Look
538	ASO0304	213.3355	-62.0808	212.410984	-61.846899	236.335934	-45.096122	312.3597658	-0.71761471	280.2937	55036.9044907407	2009-07-24 21:42:28	55038.1453935185	2009-07-26 03:29:22	504054010	44.2485	40	44.2485	44.2485	0	44.2485	2	2	0	2	1	0	0	41.0839	41.0839	107.2018	1	PROCESSED	57547.9369791667	2016-06-08 22:29:15	55415	2010-08-07 00:00:00	55048.3203819444	2009-08-05 07:41:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040112	We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504054010/	Quick Look
539	G346.6-0.2	257.5822	-40.1827	256.712432	-40.120751	260.089291	-17.167114	346.62898747	-0.22219097	278.7363	55111.704525463	2009-10-07 16:54:31	55113.1668287037	2009-10-09 04:00:14	504096010	56.7543	50	56.7543	56.7623	0	56.7703	2	2	0	2	1	0	0	42.4121	42.4121	126.3239	0	PROCESSED	57548.806724537	2016-06-09 19:21:41	54922	2009-04-01 00:00:00	55127.3766898148	2009-10-23 09:02:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504096010/	Quick Look
540	CYGNUS_LOOP_P12	313.7421	31.2725	313.223564	31.080937	328.639569	46.215284	74.99964096	-8.84356964	62.1405	53864.7943055556	2006-05-09 19:03:48	53865.1391087963	2006-05-10 03:20:19	501029010	13.5426	10	13.5426	13.5426	13.5426	13.5426	2	2	2	2	1	0	0	2.1567	2.1567	29.78	1	PROCESSED	57534.2604166667	2016-05-26 06:15:00	54394	2007-10-21 00:00:00	53914.0447916667	2006-06-28 01:04:30	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501029010/	Quick Look
541	SNR 0509-67.5	77.3855	-67.5341	77.403087	-67.594899	342.98809	-84.999306	278.15788525	-34.58671131	68.6442	53965.2623032407	2006-08-18 06:17:43	53966.1640509259	2006-08-19 03:56:14	501041010	51.2762	50	51.2762	51.2762	51.2762	51.2762	2	2	2	2	1	0	0	50.8294	50.8294	77.89	1	PROCESSED	57535.3081365741	2016-05-27 07:23:43	54526	2008-03-01 00:00:00	54020.7617592593	2006-10-12 18:16:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010072	Hot plasma in young supernova remnants (SNRs) are generally in the state of non-equilibrium ionization (NEI), hence strong L-shell lines of Si, Fe and other elements appear in soft energy band (<1keV). With the observations with Chandra and XMM, quite large ambiguity of ionization age for each element remains because of the limited energy resolution in the soft energy band. Utilizing the supreme energy resolution and background property of Suzaku/XIS, we propose the observation of the youngest type Ia SNR in the LMC, 0509-67.5. We correctly diagnose the NEI plasma of this SNR by determining the ionization age and electron temperature for each element component and constrain the ejecta structure of Type Ia SNR.	GALACTIC DIFFUSE EMISSION	5	C	HIROSHI NAKAJIMA		JAP	1	AO1	NEI PLASMA DIAGNOSTICS OF A YOUNG TYPE IA SNR:0509-67.5	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501041010/	Quick Look
542	GALACTIC CENTER	265.9791	-28.902	265.18515	-28.880549	266.454701	-5.510331	359.8343278	0.33569605	108.8002	54169.6271990741	2007-03-10 15:03:10	54170.1633564815	2007-03-11 03:55:14	501046010	25.211	25	25.227	25.211	0	25.243	2	2	0	2	1	0	0	25.0087	25.0087	46.2919	0	PROCESSED	57537.6350925926	2016-05-29 15:14:32	54736	2008-09-27 00:00:00	54179.4773842593	2007-03-20 11:27:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501046010/	Quick Look
543	73P/SW3	317.9167	24.1666	317.359719	23.9609	329.535722	38.234901	71.86402338	-16.24383714	72.7109	53868.3425	2006-05-13 08:13:12	53868.4085532407	2006-05-13 09:48:19	500013040	3.225	20	3.225	3.225	3.225	3.225	1	1	1	1	1	0	0	2.677	2.677	5.7039	0	PROCESSED	57534.2934143518	2016-05-26 07:02:31	54256	2007-06-05 00:00:00	54042.2977430556	2006-11-03 07:08:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013040/	Quick Look
544	GALACTIC CENTER	265.7083	-29.9322	264.907837	-29.909421	266.247634	-6.546909	358.83372455	-0.00453222	269.0002	54017.5695486111	2006-10-09 13:40:09	54018.2808333333	2006-10-10 06:44:24	501051010	21.869	20	21.877	21.877	21.869	21.877	2	2	2	2	1	0	0	21.1322	21.1322	61.4459	0	PROCESSED	57535.8166435185	2016-05-27 19:35:58	54735	2008-09-26 00:00:00	54053.5109953704	2006-11-14 12:15:50	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501051010/	Quick Look
545	W44	284.0351	1.3886	283.400736	1.32257	285.389988	24.082424	34.70383121	-0.41279271	90.6817	55296.8229513889	2010-04-10 19:45:03	55298.1591898148	2010-04-12 03:49:14	505004010	61.1433	60	61.1513	61.1433	0	61.1513	2	2	0	2	1	0	0	53.7129	53.7129	115.3999	2	PROCESSED	57551.2065625	2016-06-12 04:57:27	55287	2010-04-01 00:00:00	55313.4281597222	2010-04-27 10:16:33	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050002	We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505004010/	Quick Look
546	RXJ1713-3946	258.5534	-39.7289	257.686429	-39.671569	260.823727	-16.651038	347.43430559	-0.55631777	267.9997	53991.0497337963	2006-09-13 01:11:37	53991.4460300926	2006-09-13 10:42:17	501068010	21.0015	20	21.0175	21.0095	21.0015	21.0255	2	2	2	2	1	0	0	21.2093	21.2093	34.2339	1	PROCESSED	57535.5599537037	2016-05-27 13:26:20	54526	2008-03-01 00:00:00	54021.2424537037	2006-10-13 05:49:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501068010/	Quick Look
547	CYGNUS LOOP 8	313.6776	30.8178	313.157016	30.626468	328.307341	45.819556	74.60811536	-9.08900254	81.5524	55306.7979398148	2010-04-20 19:09:02	55307.2786689815	2010-04-21 06:41:17	505016010	23.5534	21	23.5614	23.5534	0	23.5694	1	1	0	1	1	0	0	20.1989	20.1989	41.5279	0	PROCESSED	57551.2800462963	2016-06-12 06:43:16	55287	2010-04-01 00:00:00	55364.2401967593	2010-06-17 05:45:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505016010/	Quick Look
548	L168_B53	153.7378	48.0763	152.957538	48.325063	136.571096	34.402104	167.64470811	53.18666692	109.5667	55519.8069328704	2010-11-19 19:21:59	55521.5828356482	2010-11-21 13:59:17	505058010	79.4999	80	79.4999	79.4999	0	79.4999	2	2	0	2	1	0	0	35.6619	35.6619	153.4218	1	PROCESSED	57554.2060763889	2016-06-15 04:56:45	55898	2011-12-03 00:00:00	55530.2748842593	2010-11-30 06:35:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050106	A dark patch extending degrees scale was found in the R4-band ROSAT All Sky Survey data from our re-analysis of the map based on the recent Suzaku results. The deficiency is small in R5 band . Strikingly the area well coincides with the dark patch in the 408 MHz emission. This indicates the low cosmic-ray and magnetic pressure of this area. We propose to observe this area to determine the temperature of the halo emission using Oxygen lines and to constrain the thermal pressure of hot interstellar medium.	GALACTIC DIFFUSE EMISSION	5	C	NORIO SEKIYA		JAP	5	AO5	DARK PATCH IN THE GALACTIC HALO X-RAY EMISSION AND ITS POSSIBLE RELATION TO RADIO SYNCHROTRON RADIATION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505058010/	Quick Look
549	DEM L 199	81.6473	-68.8371	81.71922	-68.877404	320.411618	-86.105475	279.33316137	-32.78488249	187.7916	55551.3246759259	2010-12-21 07:47:32	55552.146099537	2010-12-22 03:30:23	505042010	51.7434	50	51.7564	51.7434	0	51.7564	2	2	0	2	1	0	0	48.2079	48.2079	70.9659	0	PROCESSED	57554.4832523148	2016-06-15 11:35:53	55961	2012-02-04 00:00:00	55593.2050231482	2011-02-01 04:55:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050061	Some of the Supper bubbles (SBs), the large hot cavities created by the combined actions of strong stellar winds and supernova explosions of massive stars, have proved to be the strong emitters of non-thermal X-rays. By observing two brightest SBs (DEM L 86 and DEM L 199) in the LMC, we investigate the universality of particle acceleration in SBs, and make the conclusion if SBs are the primary acceleration cites of the galactic cosmic rays. We also investigate the energy crisis problem in SBs, that is, there is a large discrepancy between energy income (SN and stellar wind) and its outlays (thermal/kinetic energy of the shell). By estimating the thermal energies of the SB shells precisely, we measure the amount of missing energy and the conversion efficiency to the non-thermal particles.	GALACTIC DIFFUSE EMISSION	5	C	HIROSHI NAKAJIMA		JAP	5	AO5	UNIVERSALITY OF PARTICLE ACCELERATION IN SUPERBUBBLES AND SOLVING THEIR ENERGY CRISIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505042010/	Quick Look
550	LMC X-3 OFF FIELD 1	85.5783	-64.5441	85.521216	-64.565729	45.792643	-87.283954	274.09377866	-31.6918405	324.0002	53847.1442361111	2006-04-22 03:27:42	53848.0099421296	2006-04-23 00:14:19	501097010	43.6067	50	43.6067	43.6067	43.6067	43.6067	2	2	2	2	1	0	0	42.0261	42.0261	74.7459	0	PROCESSED	57533.5339583333	2016-05-25 12:48:54	54526	2008-03-01 00:00:00	53907.3335763889	2006-06-21 08:00:21	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011256	The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona.	GALACTIC DIFFUSE EMISSION	5	A	Q. DANIEL WANG		USA	1	AO1	A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501097010/	Quick Look
551	VELA SNR CB3	129.7826	-44.6964	129.353744	-44.51903	154.049323	-59.60688	263.57338638	-1.96329272	278.1748	55318.927974537	2010-05-02 22:16:17	55319.3418402778	2010-05-03 08:12:15	505070010	18.1718	20	18.1718	18.1718	0	18.1718	2	2	0	2	1	0	0	17.1544	17.1544	35.7539	1	PROCESSED	57551.3562847222	2016-06-12 08:33:03	55696	2011-05-15 00:00:00	55330.1275925926	2010-05-14 03:03:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051304	The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	5	AO5	IRON-RICH EJECTA BULLET IN THE VELA SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505070010/	Quick Look
552	G12.0-0.1	273.0232	-18.6277	272.288654	-18.640604	272.865066	4.782958	11.94868379	-0.09019508	259.2908	54375.5953819444	2007-10-02 14:17:21	54376.9863310185	2007-10-03 23:40:19	502001010	53.7521	53	53.7521	53.7521	0	53.7521	2	2	0	2	1	0	0	47.183	47.183	120.172	1	PROCESSED	57540.1741898148	2016-06-01 04:10:50	54751	2008-10-12 00:00:00	54403.1207986111	2007-10-30 02:53:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020010	We propose an observation of a supernova remnant (SNR) G12.0-0.1 with Suzaku. ASCA discovered X-ray emission from this SNR. The X-ray spectrum exhibit a power-law shape, and the radius and X-ray luminosity estimated from the ASCA results are similar to those of SN 1006, which suggests that it is a SN 1006-like SNR. However, due to the poor statistics, we could not conclude that G12.0-0.1 is SN 1006-like SNR. Precise measurements of the X-ray spectrum with the XIS will provide us with understanding the physical process in the SNR.	GALACTIC DIFFUSE EMISSION	5	B	SHIGEO YAMAUCHI		JAP	2	AO2	SUZAKU OBSERVATION OF G12.0-0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502001010/	Quick Look
553	HESS J1841-55 4	280.4555	-5.2917	279.789233	-5.340638	280.927287	17.753088	27.12788601	-0.27973073	86.6744	55648.7926273148	2011-03-28 19:01:23	55649.9633449074	2011-03-29 23:07:13	505091010	51.2539	50	51.2539	51.2539	0	51.2539	2	2	0	2	1	0	0	45.0078	45.0078	101.142	1	PROCESSED	57601.3663310185	2016-08-01 08:47:31	55287	2010-04-01 00:00:00	55666.3000115741	2011-04-15 07:12:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505091010/	Quick Look
554	RCW86_SOUTH	220.8315	-62.6734	219.843557	-62.461116	241.073682	-44.079198	315.37853465	-2.53716675	96.1597	54862.1182291667	2009-01-31 02:50:15	54863.3647569445	2009-02-01 08:45:15	503003010	54.8181	50	54.8181	54.8181	0	54.8341	2	2	0	2	1	0	0	47.3483	47.3483	107.6848	1	PROCESSED	57545.4382175926	2016-06-06 10:31:02	55329	2010-05-13 00:00:00	54880.5892361111	2009-02-18 14:08:30	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030011	Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		JAP	3	AO3	RCW86 MAPPING OBSERVATION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503003010/	Quick Look
555	THE KEPLER SNR	262.671	-21.485	261.921744	-21.447676	263.170047	1.78246	4.52284766	6.82247636	99.4153	55649.9685416667	2011-03-29 23:14:42	55653.0828356482	2011-04-02 01:59:17	505092070	133.3906	90	133.3986	133.3986	0	133.3906	2	2	0	2	1	0	0	112.2172	112.2172	269.0278	1	PROCESSED	57601.4459490741	2016-08-01 10:42:10	55287	2010-04-01 00:00:00	55666.5226736111	2011-04-15 12:32:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092070/	Quick Look
556	VELA JR P20	133.6175	-46.3272	133.188109	-46.13587	160.261964	-59.591088	266.52787238	-0.88873335	346.9997	54651.2368402778	2008-07-04 05:41:03	54651.5828009259	2008-07-04 13:59:14	503032010	16.8237	10	16.8237	16.8317	0	16.8317	1	1	0	1	1	0	0	14.7982	14.7982	29.8879	0	PROCESSED	57542.9499074074	2016-06-03 22:47:52	55036	2009-07-24 00:00:00	54665.3228125	2008-07-18 07:44:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503032010/	Quick Look
557	W49B	287.7847	9.1157	287.186344	9.032042	290.655059	31.28998	43.28157058	-0.18360003	89.2671	54919.1063888889	2009-03-29 02:33:12	54920.4689583333	2009-03-30 11:15:18	503084010	52.1549	40	52.1549	52.1549	0	52.1549	2	2	0	2	1	0	0	43.9512	43.9512	117.7099	2	PROCESSED	57547.7422685185	2016-06-08 17:48:52	55330	2010-05-14 00:00:00	54931.3622106482	2009-04-10 08:41:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030142	Observations of the W49B supernova remnant for 40 ks is proposed to reveal whether it is a remnant of an anomalous Type Ia supernova or not. To determine the type of the supernova, detailed measurement of less abundand elements such as Cr and Mn will be performed, and abundance of Ni and Ti will be examined. The abundance pattern of those elements in W49B will be compared to that of Tycho's SNR we measured by Suzaku.	GALACTIC DIFFUSE EMISSION	5	C	TORU TAMAGAWA		JAP	3	AO3	IS W49B A REMNANT OF AN ANOMALOUS TYPE IA SUPERNOVA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503084010/	Quick Look
558	GAMMACYGNI_NWSHELL1	304.9359	40.8711	304.492598	40.71257	324.526393	57.885883	78.38707497	2.60425327	82.9977	55664.4219675926	2011-04-13 10:07:38	55665.3022222222	2011-04-14 07:15:12	506017010	39.0271	40	39.0271	39.0271	0	39.0271	2	2	0	2	1	0	0	37.6965	37.6965	76.052	0	PROCESSED	57601.5010416667	2016-08-01 12:01:30	56058	2012-05-11 00:00:00	55690.9556597222	2011-05-09 22:56:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060059	We propose deep X-ray observations of outer edge of gamma Cygni SNR north-west shell with Suzaku. Radio observation shows that this SNR has shell-type structure in the north-west and south-east. High energy diffuse gamma-ray emission have been recently detected from the north-west shell by Fermi gamma-ray space telescope and VERITAS TeV telescope. Main objective of this proposal is to reveal the emission mechanisms not only in X-ray band but also in GeV and TeV bands through the extent of the X-ray emission and spectroscopy. Only Suzaku can achieve this, because the background level of XIS is very low and the broadness of the energy band.	GALACTIC DIFFUSE EMISSION	5	B	YASUYUKI TANAKA		JAP	6	AO6	SUZAKU X-RAY OBSERVATION OF OUTER EDGE OF GAMMA CYGNI SNR NORTH-WEST SHELL	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506017010/	Quick Look
559	VELA JR P6	133.325	-45.4847	132.890485	-45.294415	159.041125	-58.989018	265.75161327	-0.50306307	347.0024	54286.7508449074	2007-07-05 18:01:13	54286.9863888889	2007-07-05 23:40:24	502028010	11.5072	10	11.5312	11.5232	0	11.5072	1	1	0	1	1	0	0	8.2579	8.2579	20.3439	0	PROCESSED	57539.1055324074	2016-05-31 02:31:58	54696	2008-08-18 00:00:00	54328.3854166667	2007-08-16 09:15:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502028010/	Quick Look
560	CTB1_SW	359.716	62.4332	359.080854	62.154888	37.143182	54.514989	116.89133919	0.1796486	252.1748	55924.1262037037	2011-12-29 03:01:44	55924.6251736111	2011-12-29 15:00:15	506034010	28.9419	50	28.9419	28.9499	0	28.9499	2	2	0	2	1	0	0	25.385	25.385	43.108	0	PROCESSED	57604.2594675926	2016-08-04 06:13:38	56313	2013-01-21 00:00:00	55972.6473958333	2012-02-15 15:32:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060086	CTB 1 is an old (9 - 44 thousand years) galactic supernova remnant (SNR). The ASCA observation of CTB 1 suggested a hard X-ray emission in the 3 - 10 keV band. The hard emission may be originated in synchrotron radiation (non-thermal) or in thermal bremsstrahlung (kT ~ 3 keV). In the case of the non-thermal origin, the old SNR still accelerate electrons up to 100 TeV. On the other hand, the thermal origin indicates that very hot plasma is still kept in such an old SNR. In order to clean up the nature of the hard emission which would give a large impact for the mechanism of particle acceleration and SNR evolution, we propose the Suzaku observation of CTB 1.	GALACTIC DIFFUSE EMISSION	5	C	SHINYA NAKASHIMA		JAP	6	AO6	NON-THERMAL EMISSION FROM THE MOST ANCIENT SUPERNOVA REMNANT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506034010/	Quick Look
561	MONOGEM RING W1	100.4191	15.2834	99.703498	15.332031	100.143287	-7.791413	198.20484712	4.79777248	269.9998	55998.5603356482	2012-03-12 13:26:53	56000.0002314815	2012-03-14 00:00:20	506053010	61.1266	60	61.1267	61.1266	0	61.1266	3	2	0	2	1	0	0	59.074	59.074	124.3739	1	PROCESSED	57604.899849537	2016-08-04 21:35:47	56382	2013-03-31 00:00:00	56016.6737152778	2012-03-30 16:10:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061316	We propose to observe the oldest, nearby SNR, the Monogem Ring, with the Suzaku XIS to study the plasma conditions in two locations which are near the Galactic plane and where there is evidence of a significant interaction with cooler (10^4 - 10^5 K), denser material. We chose one pointing where the turbulent mixing of hot and cooler gas should be large, and an adjacent pointing where the mixing should be small. From our previous Suzaku observation at a region far from the plane, we derived an ionization timescale for the non-equilibrium plasma which is apparently inconsistent with the age of the SNR. Our proposed observations will allow a detailed comparison of the plasma conditions in these regions with very different histories, and initial and current conditions.	GALACTIC DIFFUSE EMISSION	5	C	PAUL PLUCINSKY		USA	6	AO6	STUDYING THE PLASMA EVOLUTION IN THE MONOGEM RING	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506053010/	Quick Look
562	G236+38 ON	146.5345	0.5057	145.892219	0.737078	148.588681	-12.195052	235.93345442	38.21375915	307.3884	55713.4761574074	2011-06-01 11:25:40	55715.0002314815	2011-06-03 00:00:20	506055010	69.8025	70	69.8025	69.8025	0	69.8025	2	2	0	2	1	0	0	64.3488	64.3488	131.674	0	PROCESSED	57602.2264351852	2016-08-02 05:26:04	56127	2012-07-19 00:00:00	55757.6954050926	2011-07-15 16:41:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061321	Interstellar clouds cast shadows in the soft X-ray background (SXRB). Observations of these shadows enable us to disentangle the various components of the SXRB. Unfortunately, to date, shadowing observations with XMM or Suzaku have only been published for three directions, all in the southern Galactic hemisphere. We propose two new pairs of on- and off-cloud shadowing observations, in order to sample the northern Galactic hemisphere. Our particular goal is to obtain accurate X-ray spectra of the Galactic halo, which we will compare with the predictions of models of galactic fountains and infalling extragalactic material.	GALACTIC DIFFUSE EMISSION	5	B	DAVID HENLEY		USA	6	AO6	UNDERSTANDING THE ORIGIN OF THE GALACTIC HALO USING SHADOWING OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506055010/	Quick Look
563	RXJ1713-3946_ID4	258.9125	-40.0131	258.042933	-39.957471	261.134722	-16.911926	347.36417887	-0.94594655	86.0017	55244.4787384259	2010-02-17 11:29:23	55244.8903587963	2010-02-17 21:22:07	504030010	22.1534	20	22.1774	22.1694	0	22.1534	2	2	0	2	1	0	0	19.7193	19.7193	35.5579	1	PROCESSED	57550.6146412037	2016-06-11 14:45:05	55622	2011-03-02 00:00:00	55256.0824768518	2010-03-01 01:58:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040021	We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009.	GALACTIC DIFFUSE EMISSION	5	B	TADAYUKI TAKAHASHI		JAP	4	AO4	STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504030010/	Quick Look
564	G292.0+1.8	171.1489	-59.2723	170.582246	-58.997353	208.114622	-55.074076	292.03159099	1.74911685	309.5957	55764.9604050926	2011-07-22 23:02:59	55765.6883449074	2011-07-23 16:31:13	506062010	43.6592	40	43.6592	43.6592	0	43.6592	2	2	0	2	1	0	0	40.2364	40.2364	62.8859	1	PROCESSED	57602.6430902778	2016-08-02 15:26:03	55652	2011-04-01 00:00:00	55785.0141782407	2011-08-12 00:20:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506062010/	Quick Look
565	FERMI_BUBBLE_S4	331.467	-46.3468	330.684504	-46.590536	315.761845	-32.186623	351.15250978	-52.26066971	44.0063	56036.1354976852	2012-04-19 03:15:07	56036.5905324074	2012-04-19 14:10:22	507012010	21.1637	20	21.1717	21.1637	0	21.1718	1	1	0	1	1	0	0	15.3816	15.3816	39.3039	0	PROCESSED	57605.2132291667	2016-08-05 05:07:03	56434	2013-05-22 00:00:00	56068.6280671296	2012-05-21 15:04:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507012010/	Quick Look
566	GC_SOUTH_3	268.18	-29.2061	267.383741	-29.195321	268.393759	-5.775192	0.56701913	-1.46906711	273.9841	56205.6096412037	2012-10-05 14:37:53	56206.6341898148	2012-10-06 15:13:14	507030010	51.7418	50	51.7498	51.7498	0	51.7418	2	2	0	2	1	0	0	52.1911	52.1911	88.5159	0	PROCESSED	57607.309537037	2016-08-07 07:25:44	56595	2013-10-30 00:00:00	56226.549212963	2012-10-26 13:10:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070042	We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation.	GALACTIC DIFFUSE EMISSION	5	A	SHINYA NAKASHIMA		JAP	7	AO7	OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507030010/	Quick Look
567	G32.8-0.1 SOUTH	282.8163	-0.2514	282.174201	-0.311644	283.889842	22.573278	32.68848527	-0.07620379	74.5004	56038.7902430556	2012-04-21 18:57:57	56039.916087963	2012-04-22 21:59:10	507036010	52.2324	50	52.2404	52.2324	0	52.2484	2	2	0	2	1	0	0	50.2432	50.2432	97.268	1	PROCESSED	57605.2444560185	2016-08-05 05:52:01	56421	2013-05-09 00:00:00	56055.0208564815	2012-05-08 00:30:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070047	A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem.	GALACTIC DIFFUSE EMISSION	5	B	AYA BAMBA		JAP	7	AO7	SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507036010/	Quick Look
568	COMET_8P_TUTTLE-P1-3	28.0473	7.5049	27.389882	7.258447	28.728614	-3.762405	148.10975305	-52.37174422	248.4997	54470.6493055556	2008-01-05 15:35:00	54470.7154861111	2008-01-05 17:10:18	502062030	1.9633	2	1.9633	1.9633	0	1.9633	1	1	0	1	1	0	0	1.905	1.905	5.718	0	PROCESSED	57540.9903935185	2016-06-01 23:46:10	54908	2009-03-18 00:00:00	54542.2294791667	2008-03-17 05:30:27	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062030/	Quick Look
569	SNR HB3 SE-A	35.6022	61.9246	34.662678	61.696985	57.575576	44.47157	133.41628397	0.91883689	247.499	56322.7203935185	2013-01-30 17:17:22	56323.4079050926	2013-01-31 09:47:23	507056010	46.748	40	46.748	46.7517	0	46.7597	2	2	0	2	1	0	0	43.9628	43.9628	59.3939	0	PROCESSED	57608.6541666667	2016-08-08 15:42:00	56709	2014-02-21 00:00:00	56342.6336921296	2013-02-19 15:12:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071316	We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective.	GALACTIC DIFFUSE EMISSION	5	C	JUNICHIRO KATSUTA		USA	7	AO7	SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507056010/	Quick Look
570	SGR B	266.8769	-28.4429	266.085661	-28.425809	267.234018	-5.031789	0.6365241	-0.09758916	267.0001	56556.6453472222	2013-09-21 15:29:18	56559.2640740741	2013-09-24 06:20:16	508018010	101.9558	100	101.9558	101.9558	0	101.9558	2	2	0	2	1	0	0	87.894	87.894	226.2438	0	PROCESSED	57612.7499768518	2016-08-12 17:59:58	56956	2014-10-26 00:00:00	56588.5828125	2013-10-23 13:59:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080043	X-ray emissions from giant molecular clouds (X-ray reflection nebula) in the Galactic center region show past activity of the super-massive black hole, Sagittarius (Sgr) A. Using Suzaku, we have found that Sgr A had been in the active phase for almost a thousand years and dropped down to the quiescent level tens of years ago. However, no detailed information during the active phase and transition has been obtained from observations to study a mechanism of the sudden phase change. We aim to observe new information about time variability and relative positions from X-ray reflection nebulae to find the past light curve of Sgr A*. This work will be the grand sum for the Suzaku observation of the Galactic center.	GALACTIC DIFFUSE EMISSION	5	A	MASAYOSHI NOBUKAWA		JAP	8	AO8	PAST HISTORY OF THE SUPER-MASSIVE BLACK HOLE IN THE GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508018010/	Quick Look
571	JUPITER	104.5549	23.0543	103.799265	23.122478	103.371966	0.286476	192.85746904	11.70034918	267.1462	56767.7816087963	2014-04-20 18:45:31	56768.1147916667	2014-04-21 02:45:18	508023130	10.0906	160	10.0986	10.0986	0	10.0906	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57614.9649652778	2016-08-14 23:09:33	57212	2015-07-09 00:00:00	56782.5091782407	2014-05-05 12:13:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023130/	Quick Look
572	G359.0-0.9 S	266.8698	-30.3116	266.066627	-30.294444	267.268772	-6.900137	359.03431589	-1.05952932	101.9997	56724.8167013889	2014-03-08 19:36:03	56726.0627662037	2014-03-10 01:30:23	508059010	53.4961	50	53.4961	53.5031	0	53.5201	1	1	0	1	1	0	0	47.9921	47.9921	107.6559	1	PROCESSED	57614.0007175926	2016-08-14 00:01:02	57106	2015-03-25 00:00:00	56740.7217013889	2014-03-24 17:19:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080113	We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	8	AO8	FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508059010/	Quick Look
573	RX J1713 CENTER	258.5686	-39.6657	257.702123	-39.608442	260.830462	-16.587092	347.49241435	-0.52884605	86.0002	56713.2203125	2014-02-25 05:17:15	56714.6669212963	2014-02-26 16:00:22	508068010	82.0615	80	82.0695	82.0695	0	82.0615	2	2	0	2	1	0	0	34.8059	34.8059	50.3319	0	PROCESSED	57613.9125231482	2016-08-13 21:54:02	57089	2015-03-08 00:00:00	56723.6064699074	2014-03-07 14:33:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081313	Detecting thermal emission and determining the ambient density are the missing keys to constrain hadronic acceleration in X-ray synchrotron-dominated SNRs. In the prototypical CR accelerator RX J1713.7-3946, X-ray thermal emission has been sought for over a decade, without success. Deep Suzaku observations will constrain either the conditions of the ambient medium in which the SNR is evolving, or the SN progenitor type (core-collapse or thermonuclear) and nucleosynthesis yield.	GALACTIC DIFFUSE EMISSION	5	B	FABIO ACERO		USA	8	AO8	STUDY OF THE THERMAL EMISSION IN THE SYNCHROTRON DOMINATED SNR RX J1713.7-3946	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508068010/	Quick Look
574	COMET_8P_TUTTLE-P2_BGD-1	40.599	-37.8517	40.099004	-38.063935	20.76393	-50.124108	244.68396515	-64.39213957	254.2787	54492.4296643518	2008-01-27 10:18:43	54492.562662037	2008-01-27 13:30:14	502064010	6.5707	5	6.5707	6.6024	0	6.5867	1	1	0	1	1	0	0	6.6293	6.6293	11.4879	0	PROCESSED	57541.4243518518	2016-06-02 10:11:04	54912	2009-03-22 00:00:00	54546.2413888889	2008-03-21 05:47:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502064010/	Quick Look
575	CTB109 SOUTHWEST	345.0971	58.7572	344.575762	58.488555	23.478605	56.879692	108.94859975	-1.06655489	252.0045	55909.1993287037	2011-12-14 04:47:02	55910.0807407407	2011-12-15 01:56:16	506038010	41.3824	40	41.3904	41.3824	0	41.3984	2	2	0	2	1	0	0	38.779	38.779	76.1358	0	PROCESSED	57604.1454282407	2016-08-04 03:29:25	56289	2012-12-28 00:00:00	55921.9811574074	2011-12-26 23:32:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060100	Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations.	GALACTIC DIFFUSE EMISSION	5	C	TOSHIO NAKANO		JAP	6	AO6	SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506038010/	Quick Look
576	ARC1	40.8605	-42.0069	40.383748	-42.218277	17.737941	-53.844666	253.28744097	-62.75503946	235.1247	54480.7980787037	2008-01-15 19:09:14	54482.7640509259	2008-01-17 18:20:14	502070010	104.3694	100	104.3774	104.3854	0	104.3694	2	2	0	2	1	0	0	115.4202	115.4202	169.8377	3	PROCESSED	57541.3640277778	2016-06-02 08:44:12	54860	2009-01-29 00:00:00	54490.7270717593	2008-01-25 17:26:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021222	Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants.	GALACTIC DIFFUSE EMISSION	5	C	ROBIN SHELTON		USA	2	AO2	A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502070010/	Quick Look
577	W49B	287.784	9.1149	287.185641	9.031245	290.654125	31.289286	43.28054167	-0.18335704	82.0063	57131.6619444445	2015-04-19 15:53:12	57133.5779513889	2015-04-21 13:52:15	509001040	67.3182	400	67.3182	67.3182	0	67.3262	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.0264699074	2016-08-18 00:38:07	56748	2014-04-01 00:00:00	57224.4531481482	2015-07-21 10:52:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090007	W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	9	AO9	DEEP OBSERVATIONS OF W49B	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001040/	Quick Look
578	VELA PWN GEV1	127.6995	-44.6062	127.276202	-44.43674	151.392903	-60.265182	262.61398048	-3.09706524	119.7191	56985.3954282407	2014-11-24 09:29:25	56985.8502546296	2014-11-24 20:24:22	509011010	19.1492	15	19.1572	19.1652	0	19.1492	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.8102893518	2016-08-16 19:26:49	57365	2015-12-09 00:00:00	57009.4123726852	2014-12-18 09:53:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090046	We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	9	AO9	X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509011010/	Quick Look
579	G166.0+4.3_NW	81.4339	42.9094	80.537947	42.865797	83.349134	19.666732	166.05797128	4.14809941	85.1436	56920.3100347222	2014-09-20 07:26:27	56921.2397106482	2014-09-21 05:45:11	509023010	39.7982	40	39.7982	42.0339	0	42.0259	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5613078704	2016-08-16 13:28:17	57298	2015-10-03 00:00:00	56940.6722569444	2014-10-10 16:08:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090092	Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation.	GALACTIC DIFFUSE EMISSION	5	A	AKIHIRO TAKATA		JAP	9	AO9	G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509023010/	Quick Look
580	CIZA J1358.9-4750_SW	209.5053	-47.9232	208.715208	-47.679899	225.712458	-33.34381	314.31638856	13.47131455	293	56882.719537037	2014-08-13 17:16:08	56883.5528356482	2014-08-14 13:16:05	509027010	42.0308	40	42.0308	42.0548	0	42.0388	2	2	0	2	1	0	0	7.0109	7.0109	14.276	0	PROCESSED	57616.4982175926	2016-08-16 11:57:26	57267	2015-09-02 00:00:00	56898.5152662037	2014-08-29 12:21:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090102	Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS.	GALACTIC DIFFUSE EMISSION	5	B	YUICHI KATO		JAP	9	AO9	OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509027010/	Quick Look
581	ARC_BACKGROUND	39.8321	-35.8483	39.320146	-36.062945	21.353527	-48.064568	240.48423372	-65.50115915	257.6627	54496.6274537037	2008-01-31 15:03:32	54499.812662037	2008-02-03 19:30:14	502072010	0	100	0	0	0	0	0	0	0	0	1	0	0	105.161	105.161	275.1537	4	PROCESSED	57541.5227314815	2016-06-02 12:32:44	54883	2009-02-21 00:00:00	54515.6371875	2008-02-19 15:17:33	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021222	Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants.	GALACTIC DIFFUSE EMISSION	5	C	ROBIN SHELTON		USA	2	AO2	A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502072010/	Quick Look
582	MBM20	68.9409	-14.6227	68.368213	-14.724058	64.473913	-36.217726	211.39642208	-36.55928879	252.4258	54507.612025463	2008-02-11 14:41:19	54510.6980439815	2008-02-14 16:45:11	502075010	107.0668	100	107.0668	107.0668	0	107.0668	2	2	0	2	1	0	0	92.8036	92.8036	266.6036	2	PROCESSED	57541.6362847222	2016-06-02 15:16:15	54889	2009-02-27 00:00:00	54522.4496527778	2008-02-26 10:47:30	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021224	We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source.	GALACTIC DIFFUSE EMISSION	5	B	MASSIMILIANO GALEAZZI		USA	2	AO2	STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502075010/	Quick Look
583	3C 396	285.987	5.4347	285.37156	5.359452	288.059681	27.878529	39.1930056	-0.29514711	64.6066	56773.2792592593	2014-04-26 06:42:08	56775.1223726852	2014-04-28 02:56:13	509038010	82.7922	80	82.7922	82.7922	0	82.7922	2	2	0	2	1	0	0	1.0111	1.0111	1.744	0	PROCESSED	57614.9978703704	2016-08-14 23:56:56	57157	2015-05-15 00:00:00	56789.6241782407	2014-05-12 14:58:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091315	We propose to conduct Suzaku observations of the Galactic supernova remnants (SNRs) Kes 69 (G21.8-0.6) and 3C 396 (G39.2-0.3). These SNRs were detected in the infrared by Spitzer and their infrared colors suggest that shocked molecules produce the observed emission. Published analyses of the X-ray emission from these SNRs (along with our own analysis of archival XMM-Newton and Chandra observations of these sources) reveals that the emission from both Kes 69 and 3C 396 is thermal and that they may both be mixed-morphology SNRs (MMSNRs) but deeper observations are needed to clarify their X-ray spectral properties. In particular, we will investigate whether these X-ray emitting plasmas are overionized, which is observed for other MMSNRs.	GALACTIC DIFFUSE EMISSION	5	B	THOMAS PANNUTI		USA	9	AO9	SUZAKU OBSERVATIONS OF THE SPITZER-DETECTED GALACTIC SUPERNOVA REMNANTS KES 69 (G21.8-0.6) AND 3C 396 (G39.2-0.3)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509038010/	Quick Look
584	MBM20	68.9408	-14.6235	68.368117	-14.724858	64.47362	-36.218496	211.39729046	-36.55969232	255.8156	57069.9923842593	2015-02-16 23:49:02	57071.9654050926	2015-02-18 23:10:11	509076010	81.154	80	81.154	81.162	0	81.162	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.624537037	2016-08-17 14:59:20	56748	2014-04-01 00:00:00	57083.4173032407	2015-03-02 10:00:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096001	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	9	AO9	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509076010/	Quick Look
585	VELA JR P34	132.1138	-46.9499	131.694344	-46.763927	159.20149	-60.674913	266.35035002	-2.0812575	347.0005	54656.0096990741	2008-07-09 00:13:58	54656.2634143518	2008-07-09 06:19:19	503046010	11.0421	10	11.0581	11.0421	0	11.0581	2	2	0	2	1	0	0	11.1306	11.1306	21.916	0	PROCESSED	57543.0076967593	2016-06-04 00:11:05	55037	2009-07-25 00:00:00	54670.2236342593	2008-07-23 05:22:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503046010/	Quick Look
586	VELA JR P37	132.6136	-47.1701	132.194095	-46.982326	160.029329	-60.672793	266.73640279	-1.95651055	346.9993	54656.9174768518	2008-07-09 22:01:10	54657.2418287037	2008-07-10 05:48:14	503049010	12.5294	10	12.5414	12.5294	0	12.5454	2	2	0	2	1	0	0	12.8527	12.8527	28.02	0	PROCESSED	57543.0205671296	2016-06-04 00:29:37	55037	2009-07-25 00:00:00	54670.278900463	2008-07-23 06:41:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503049010/	Quick Look
587	WESTERLUND 2	156.0088	-57.7448	155.54834	-57.490842	195.724597	-59.560466	284.2643696	-0.3172737	343.7602	54687.6527199074	2008-08-09 15:39:55	54689.327962963	2008-08-11 07:52:16	503053010	73.67	100	73.67	73.67	0	73.67	2	2	0	2	1	0	0	86.5776	86.5776	144.7298	0	PROCESSED	57543.2480555556	2016-06-04 05:57:12	55252	2010-02-25 00:00:00	54706.476412037	2008-08-28 11:26:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030059	Although young open clusters with many massive stars have been recognized as gamma-ray sources, the emission mechanism of the gamma-ray is hardly known. We propose a Suzaku observation of an open cluster Westerlund 2 (RCW 49), from which gamma-ray emission has been detected with H.E.S.S. We observe this cluster to detect X-ray nonthermal emission from open clusters with TeV gamma-ray emission for the first time. We try to find out whether the emission comes from electrons or protons, and discuss the particle acceleration in open clusters.	GALACTIC DIFFUSE EMISSION	5	A	YUTAKA FUJITA		JAP	3	AO3	NONTHERMAL EMISSION FROM AN OPEN CLUSTER WESTERLUND 2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503053010/	Quick Look
588	WESTERLUND 2	155.9878	-57.7462	155.527496	-57.492284	195.71117	-59.569482	284.25564056	-0.32444098	166.5036	54866.5949189815	2009-02-04 14:16:41	54867.1669444444	2009-02-05 04:00:24	503053020	33.4924	30	33.5004	33.4924	0	33.5004	2	2	0	2	1	0	0	32.073	32.073	49.4159	1	PROCESSED	57545.4584606482	2016-06-06 11:00:11	55329	2010-05-13 00:00:00	54880.5574189815	2009-02-18 13:22:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030059	Although young open clusters with many massive stars have been recognized as gamma-ray sources, the emission mechanism of the gamma-ray is hardly known. We propose a Suzaku observation of an open cluster Westerlund 2 (RCW 49), from which gamma-ray emission has been detected with H.E.S.S. We observe this cluster to detect X-ray nonthermal emission from open clusters with TeV gamma-ray emission for the first time. We try to find out whether the emission comes from electrons or protons, and discuss the particle acceleration in open clusters.	GALACTIC DIFFUSE EMISSION	5	A	YUTAKA FUJITA		JAP	3	AO3	NONTHERMAL EMISSION FROM AN OPEN CLUSTER WESTERLUND 2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503053020/	Quick Look
589	HESS J1745-303B	266.0577	-30.545	265.253177	-30.523904	266.569275	-7.150762	358.47050833	-0.58308172	102.2921	55254.6768634259	2010-02-27 16:14:41	55255.9515509259	2010-02-28 22:50:14	504002010	53.0609	50	53.0609	53.0609	0	53.0609	2	2	0	2	1	0	0	46.585	46.585	110.1219	1	PROCESSED	57550.7606481482	2016-06-11 18:15:20	55636	2011-03-16 00:00:00	55267.2715856482	2010-03-12 06:31:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040001	The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	4	AO4	DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504002010/	Quick Look
590	ASO0218	157.1332	-58.313	156.668691	-58.056852	197.346686	-59.525927	285.06973918	-0.48663651	315.2825	55020.3423148148	2009-07-08 08:12:56	55020.9467476852	2009-07-08 22:43:19	504045010	22.8449	20	22.8449	22.8449	0	22.8449	2	2	0	2	1	0	0	21.1544	21.1544	52.2179	1	PROCESSED	57547.7933680556	2016-06-08 19:02:27	55400	2010-07-23 00:00:00	55034.2716898148	2009-07-22 06:31:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 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 DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504045010/	Quick Look
591	GALACTIC_BULGE13	264.5912	-32.1955	263.77613	-32.167278	265.360141	-8.841295	356.40747371	-0.39354159	92.0351	55635.5794907407	2011-03-15 13:54:28	55636.621099537	2011-03-16 14:54:23	505082010	48.4969	50	48.5129	48.5129	0	48.4969	2	2	0	2	1	0	0	41.255	41.255	89.9798	0	PROCESSED	57601.201412037	2016-08-01 04:50:02	55287	2010-04-01 00:00:00	55648.3385763889	2011-03-28 08:07:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505082010/	Quick Look
592	CYGNUS LOOP 6	314.1656	31.2305	313.646001	31.037451	329.094604	46.032553	75.19999907	-9.14964477	81.8988	55301.8924189815	2010-04-15 21:25:05	55302.1398148148	2010-04-16 03:21:20	505014010	12.4623	10	12.4783	12.4623	0	12.4783	1	1	0	1	1	0	0	12.0683	12.0683	21.3599	0	PROCESSED	57551.2257060185	2016-06-12 05:25:01	55287	2010-04-01 00:00:00	55362.3410532407	2010-06-15 08:11:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505014010/	Quick Look
593	SNR G106.3+2.7 P3	336.5055	60.7692	336.063779	60.514367	20.620799	61.417005	106.0859109	2.74547808	12.2692	55424.0215509259	2010-08-16 00:31:02	55424.9841782407	2010-08-16 23:37:13	505073010	50.4548	50	50.4628	50.4548	0	50.4632	2	2	0	2	1	0	0	50.2105	50.2105	83.1639	1	PROCESSED	57553.1155439815	2016-06-14 02:46:23	55805	2011-09-01 00:00:00	55439.1312037037	2010-08-31 03:08:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051305	After two decades searching for the origin of the GeV emission from 3EG J2227+6122, it is now identified with PSR J2229+6114 and its PWN.~This highly energetic young pulsar lies within the arcmin diameter Boomerang radio nebula. Now, recently discovered nearby extended TeV emission suggest a second Vela-like "cocoon" feed by relic electrons from the PWN, blowing out the vast degree-scale radio feature.~Interactions of the SNR shock front with overlapping molecular cloud material can also contribute in the gamma-ray production.~An XIS mosaic will allow us to search for soft and hard X-ray emission similar to Vela's "Cocoon" and resolve the nature of the TeV emission and its connection to the Boomerang and the radio feature.	GALACTIC DIFFUSE EMISSION	5	C	ESTER ALIU		USA	5	AO5	ORIGIN OF THE VHE GAMMA-RAY EMISSION FROM SNR G106.3+2.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505073010/	Quick Look
594	CYGNUS LOOP 12	313.6077	30.3526	313.085044	30.161518	327.967179	45.415269	74.20451075	-9.33661335	82.0022	55329.1256944444	2010-05-13 03:01:00	55329.8391666667	2010-05-13 20:08:24	505020010	27.8427	28	27.8507	27.8507	0	27.8427	2	2	0	2	1	0	0	21.0522	21.0522	61.64	0	PROCESSED	57551.5093055556	2016-06-12 12:13:24	55287	2010-04-01 00:00:00	55393.4203009259	2010-07-16 10:05:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505020010/	Quick Look
595	FVW319.8+0.3_BGD	225.4141	-58.3766	224.455219	-58.179449	241.611855	-39.24635	319.32044374	0.28957352	278.3765	55413.9313888889	2010-08-05 22:21:12	55414.6724768518	2010-08-06 16:08:22	505030010	51.6262	50	51.6262	51.6636	0	51.6476	2	2	0	2	1	0	0	40.0503	40.0503	64.0179	1	PROCESSED	57552.8534837963	2016-06-13 20:29:01	55793	2011-08-20 00:00:00	55427.2012152778	2010-08-19 04:49:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050010	Forbidden-velocity wings (FVWs) are unknown HI clouds with high velocity dispersion. They could be old supernova remnants or star-forming bubbles, although the origin is unknown. Recently, TeV gamma-rays have been detected from one of the FVWs, FVW319.8+0.3, implying that it is a cosmic-ray accelerator. We will investigate this FVW with low-background observations of Suzaku, in order to search for thermal emission from the undiscovered supernova remnant. It is not only the first discovery of X-rays from FVWs, but also the first clue of the cosmic-ray acceleration in FVWs. Even if we could detect nothing, we can conclude that this source is a kind of gdark particle accelerators h with the proposed exposure.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	5	AO5	SEARCHING FOR COSMIC ACCELERATION IN A FORBIDDEN-VELOCITY WING: A NEW OLD SUPERNOVA REMNANT ?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505030010/	Quick Look
596	DEM L 86	77.4674	-68.8946	77.532288	-68.954899	328.060855	-84.723884	279.75652902	-34.25087364	194.4731	55552.1478703704	2010-12-22 03:32:56	55552.9495601852	2010-12-22 22:47:22	505041010	51.4681	50	51.4997	51.4997	0	51.4681	2	2	0	2	1	0	0	44.2589	44.2589	69.2579	0	PROCESSED	57554.4839236111	2016-06-15 11:36:51	55973	2012-02-16 00:00:00	55607.0926851852	2011-02-15 02:13:28	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050061	Some of the Supper bubbles (SBs), the large hot cavities created by the combined actions of strong stellar winds and supernova explosions of massive stars, have proved to be the strong emitters of non-thermal X-rays. By observing two brightest SBs (DEM L 86 and DEM L 199) in the LMC, we investigate the universality of particle acceleration in SBs, and make the conclusion if SBs are the primary acceleration cites of the galactic cosmic rays. We also investigate the energy crisis problem in SBs, that is, there is a large discrepancy between energy income (SN and stellar wind) and its outlays (thermal/kinetic energy of the shell). By estimating the thermal energies of the SB shells precisely, we measure the amount of missing energy and the conversion efficiency to the non-thermal particles.	GALACTIC DIFFUSE EMISSION	5	C	HIROSHI NAKAJIMA		JAP	5	AO5	UNIVERSALITY OF PARTICLE ACCELERATION IN SUPERBUBBLES AND SOLVING THEIR ENERGY CRISIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505041010/	Quick Look
597	VELA SNR CB1	130.2067	-44.4709	129.774891	-44.291952	154.339696	-59.260079	263.57895082	-1.58638955	294.2634	55318.1574074074	2010-05-02 03:46:40	55318.5738425926	2010-05-02 13:46:20	505068010	23.6665	20	23.6665	23.678	0	23.6665	1	1	0	1	1	0	0	18.818	18.818	35.9759	1	PROCESSED	57551.3448842593	2016-06-12 08:16:38	55696	2011-05-15 00:00:00	55330.1358449074	2010-05-14 03:15:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051304	The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	5	AO5	IRON-RICH EJECTA BULLET IN THE VELA SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505068010/	Quick Look
598	HESS J1841-55 2	280.1473	-5.9564	279.477798	-6.003856	280.554771	17.113097	26.39650339	-0.31125339	87.3564	55646.4452777778	2011-03-26 10:41:12	55647.6391550926	2011-03-27 15:20:23	505089010	50.0053	50	50.0304	50.0053	0	50.0304	3	2	0	2	1	0	0	43.1789	43.1789	103.1139	0	PROCESSED	57601.3264236111	2016-08-01 07:50:03	55287	2010-04-01 00:00:00	55658.2084606482	2011-04-07 05:00:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505089010/	Quick Look
599	JUPITER	28.7092	10.4688	28.044402	10.223855	30.381154	-1.215152	147.29554938	-49.38035583	249.1847	55930.8245717593	2012-01-04 19:47:23	55931.8508564815	2012-01-05 20:25:14	506006020	35.518	160	35.522	35.518	0	35.526	2	2	0	2	1	0	0	34.367	34.367	88.6599	0	PROCESSED	57604.3110185185	2016-08-04 07:27:52	56316	2013-01-24 00:00:00	55946.2294097222	2012-01-20 05:30:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060017	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter.	GALACTIC DIFFUSE EMISSION	5	B	KUMI ISHIKAWA		JAP	6	AO6	STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006020/	Quick Look
600	CTB1_NE	0.2869	62.6043	359.6465	62.325973	37.675416	54.459267	117.18345572	0.29518062	253.7193	55923.0281134259	2011-12-28 00:40:29	55924.1251736111	2011-12-29 03:00:15	506035010	52.666	50	52.666	52.666	0	52.666	2	2	0	2	1	0	0	48.3108	48.3108	94.7759	3	PROCESSED	57604.2722569444	2016-08-04 06:32:03	56313	2013-01-21 00:00:00	55972.6734490741	2012-02-15 16:09:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060086	CTB 1 is an old (9 - 44 thousand years) galactic supernova remnant (SNR). The ASCA observation of CTB 1 suggested a hard X-ray emission in the 3 - 10 keV band. The hard emission may be originated in synchrotron radiation (non-thermal) or in thermal bremsstrahlung (kT ~ 3 keV). In the case of the non-thermal origin, the old SNR still accelerate electrons up to 100 TeV. On the other hand, the thermal origin indicates that very hot plasma is still kept in such an old SNR. In order to clean up the nature of the hard emission which would give a large impact for the mechanism of particle acceleration and SNR evolution, we propose the Suzaku observation of CTB 1.	GALACTIC DIFFUSE EMISSION	5	C	SHINYA NAKASHIMA		JAP	6	AO6	NON-THERMAL EMISSION FROM THE MOST ANCIENT SUPERNOVA REMNANT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506035010/	Quick Look
601	W28WEST	269.8372	-23.6072	269.074768	-23.604556	269.841247	-0.166403	6.15250357	0.06606197	270.1135	55844.0583217593	2011-10-10 01:23:59	55848.1342708333	2011-10-14 03:13:21	506036010	151.0892	150	151.0972	151.0892	0	151.0923	2	2	0	2	1	0	0	128.9797	128.9797	352.1259	2	PROCESSED	57603.4758449074	2016-08-03 11:25:13	56240	2012-11-09 00:00:00	55872.5113425926	2011-11-07 12:16:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060095	W28 is a mixed-morphology supernova remnant (MM SNR). Recently, GeV and TeV gamma-ray emission have been detected from the eastern edge of W28. On the other hand, we have observed the central region of W28 and have detected an over-ionized plasma, which can not be produced in the canonical evolution of SNRs. Several SNRs have been turned out to host a over-ionized plasma. All of them are MM SNR and are showing GeV and/or TeV emission. This indicates that there are some physical connections between the existence of high-energy cosmic rays and over-ionized plasma. W28 is the best place to study this possible connection due to the large apparent size. Thus, we propose Suzaku observation of western region of W28, which has not been covered by the previous mapping observations.	GALACTIC DIFFUSE EMISSION	5	A	MAKOTO SAWADA		JAP	6	AO6	THE SNR W28 - SEARCHING FOR THE PHYSICAL CONNECTION BETWEEN HIGH-ENERGY COSMIC RAYS AND OVER-IONIZED PLASMA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506036010/	Quick Look
602	MONOGEM RING W2	97.483	17.0349	96.757694	17.069404	97.197447	-6.219287	195.35325463	3.08684005	270	56001.1430439815	2012-03-15 03:25:59	56002.5487384259	2012-03-16 13:10:11	506054010	62.5933	60	62.5933	62.5933	0	62.5933	2	2	0	2	1	0	0	59.9669	59.9669	121.4439	1	PROCESSED	57604.9251967593	2016-08-04 22:12:17	56385	2013-04-03 00:00:00	56019.3467592593	2012-04-02 08:19:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061316	We propose to observe the oldest, nearby SNR, the Monogem Ring, with the Suzaku XIS to study the plasma conditions in two locations which are near the Galactic plane and where there is evidence of a significant interaction with cooler (10^4 - 10^5 K), denser material. We chose one pointing where the turbulent mixing of hot and cooler gas should be large, and an adjacent pointing where the mixing should be small. From our previous Suzaku observation at a region far from the plane, we derived an ionization timescale for the non-equilibrium plasma which is apparently inconsistent with the age of the SNR. Our proposed observations will allow a detailed comparison of the plasma conditions in these regions with very different histories, and initial and current conditions.	GALACTIC DIFFUSE EMISSION	5	C	PAUL PLUCINSKY		USA	6	AO6	STUDYING THE PLASMA EVOLUTION IN THE MONOGEM RING	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506054010/	Quick Look
603	FERMI_BUBBLE_S2	330.2693	-46.4894	329.48073	-46.73026	314.804008	-31.978019	351.28666586	-51.42688059	44.0074	56035.2081018518	2012-04-18 04:59:40	56035.6736921296	2012-04-18 16:10:07	507010010	20.3496	20	20.3576	20.3496	0	20.3648	2	2	0	2	1	0	0	14.278	14.278	40.2139	0	PROCESSED	57605.1975231482	2016-08-05 04:44:26	56420	2013-05-08 00:00:00	56049.1880555556	2012-05-02 04:30:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507010010/	Quick Look
604	VELA JR P31	133.8003	-46.8845	133.374404	-46.692518	161.076222	-59.989175	267.03483855	-1.15221367	347.0003	54655.085	2008-07-08 02:02:24	54655.3273032407	2008-07-08 07:51:19	503043010	11.2095	10	11.2175	11.2255	0	11.2095	1	1	0	1	1	0	0	11.542	11.542	20.9279	0	PROCESSED	57542.9998263889	2016-06-03 23:59:45	55048	2009-08-05 00:00:00	54679.372974537	2008-08-01 08:57:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503043010/	Quick Look
605	LDN1563	75.5223	13.867	74.815457	13.795738	75.781245	-8.862376	187.14890409	-16.70886793	81.7388	56161.9528356482	2012-08-22 22:52:05	56164.0488194444	2012-08-25 01:10:18	507078010	78.6693	80	78.6693	78.6693	0	78.6693	2	2	0	2	1	0	0	69.6801	69.6801	181.0619	0	PROCESSED	57606.963275463	2016-08-06 23:07:07	56018	2012-04-01 00:00:00	56212.8492476852	2012-10-12 20:22:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076003	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	7	AO7	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507078010/	Quick Look
606	RX J1713.7-3946 NE	258.6449	-39.4419	257.780148	-39.385009	260.872484	-16.359233	347.70840856	-0.44579664	85.9991	56714.667349537	2014-02-26 16:00:59	56716.5279513889	2014-02-28 12:40:15	508017010	100.6728	100	100.7048	100.6968	0	100.6728	2	2	0	2	1	0	0	104.394	104.394	160.7277	1	PROCESSED	57613.9490162037	2016-08-13 22:46:35	57093	2015-03-12 00:00:00	56727.6718865741	2014-03-11 16:07:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080029	We proposed Suzaku observation of a thermal emission line in the young TeV gamma-ray SNR RX J1713.7-3946. Most recently, we found the candidate of thermal emission line toward North-East of the SNR analyzed with Suzaku archive data. The region is present in the vicinity of the small molecular cloud interacts with the SNR shock wave. Main purpose is significant detection of the Si line about 5 sigma. This observation will be observable only with Suzaku and lead to a large step forward on cosmic-ray acceleration and shock-cloud interaction in the SNR.	GALACTIC DIFFUSE EMISSION	5	A	HIDETOSHI SANO		JAP	8	AO8	SUZAKU OBSERVATION OF A THERMAL EMISSION LINE IN THE SNR RX J1713.7-3946	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508017010/	Quick Look
607	JUPITER	103.9685	23.1027	103.212311	23.168111	102.830346	0.281775	192.5818164	11.23089407	264.4391	56763.3891666667	2014-04-16 09:20:24	56763.722349537	2014-04-16 17:20:11	508023050	14.3106	160	14.3106	14.3207	0	14.3207	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57614.9511111111	2016-08-14 22:49:36	57212	2015-07-09 00:00:00	56782.4912731482	2014-05-05 11:47:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023050/	Quick Look
608	VELA JR WEST2	131.7715	-45.9871	131.345884	-45.80238	157.754454	-59.989666	265.452568	-1.6600557	116.213	56619.4434490741	2013-11-23 10:38:34	56620.0800115741	2013-11-24 01:55:13	508037010	29.185	30	29.193	29.201	0	29.185	2	2	0	2	1	0	0	35.0652	35.0652	54.9859	1	PROCESSED	57613.3840277778	2016-08-13 09:13:00	56995	2014-12-04 00:00:00	56629.6443055556	2013-12-03 15:27:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080082	We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution.	GALACTIC DIFFUSE EMISSION	5	C	HIDETOSHI SANO		JAP	8	AO8	FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508037010/	Quick Look
609	G359.0-0.9 NE	266.7211	-30.1578	265.918955	-30.139926	267.135952	-6.749255	359.09932581	-0.86996543	100.9984	56720.9624537037	2014-03-04 23:05:56	56722.041875	2014-03-06 01:00:18	508057010	49.8156	50	49.8156	49.8396	0	49.8236	3	2	0	2	1	0	0	45.0097	45.0097	93.2479	1	PROCESSED	57613.9450925926	2016-08-13 22:40:56	57102	2015-03-21 00:00:00	56740.6678009259	2014-03-24 16:01:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080113	We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	8	AO8	FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508057010/	Quick Look
610	VELA PWN S1	128.1818	-46.8811	127.77491	-46.709753	154.389152	-62.054406	264.65396784	-4.16648977	122.1894	56988.5541087963	2014-11-27 13:17:55	56988.8905324074	2014-11-27 21:22:22	509017010	15.4638	15	15.4638	15.4878	0	15.7838	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.8238194444	2016-08-16 19:46:18	57368	2015-12-12 00:00:00	57002.4344328704	2014-12-11 10:25:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090046	We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	9	AO9	X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509017010/	Quick Look
611	G166.0+4.3_NE	81.7708	42.9893	80.873891	42.947312	83.615806	19.731256	166.12860985	4.39756168	84.8043	56919.0138773148	2014-09-19 00:19:59	56920.3092824074	2014-09-20 07:25:22	509022010	54.3942	60	54.3942	61.5931	0	61.5931	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5656134259	2016-08-16 13:34:29	57296	2015-10-01 00:00:00	56940.6693981482	2014-10-10 16:03:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090092	Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation.	GALACTIC DIFFUSE EMISSION	5	A	AKIHIRO TAKATA		JAP	9	AO9	G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509022010/	Quick Look
612	OFF-FIELD5	318.3256	-10.4856	317.650019	-10.692475	317.524522	5.342962	39.92155172	-36.21028826	81.4906	56787.0661226852	2014-05-10 01:35:13	56789.4168171296	2014-05-12 10:00:13	509046010	80.908	80	80.908	80.908	0	80.908	2	2	0	2	1	0	0	71.3404	71.3404	203.0697	2	PROCESSED	57615.126724537	2016-08-15 03:02:29	56748	2014-04-01 00:00:00	56806.674212963	2014-05-29 16:10:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091321	Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma.	GALACTIC DIFFUSE EMISSION	5	A	ANJALI GUPTA		USA	9	AO9	CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509046010/	Quick Look
613	RXJ1713-3946	258.942	-39.4278	258.077115	-39.372323	261.109643	-16.326699	347.8535904	-0.62405701	268.0013	53998.4433912037	2006-09-20 10:38:29	53998.8467476852	2006-09-20 20:19:19	501071010	21.1741	20	21.1741	21.1981	21.1901	21.1821	1	1	1	1	1	0	0	18.3387	18.3387	34.8399	0	PROCESSED	57535.634537037	2016-05-27 15:13:44	54526	2008-03-01 00:00:00	54020.8878009259	2006-10-12 21:18:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501071010/	Quick Look
614	73P/SW3	17.8996	-9.1693	17.272719	-9.434717	12.886588	-15.48163	138.7272506	-71.42013328	59.3998	53893.8025	2006-06-07 19:15:36	53893.8689699074	2006-06-07 20:51:19	500014030	3.2361	35	3.2361	3.2361	3.2361	3.2361	1	1	1	1	1	0	0	2.4331	2.4331	5.7359	0	PROCESSED	57534.5821875	2016-05-26 13:58:21	54267	2007-06-16 00:00:00	54052.5088310185	2006-11-13 12:12:43	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014030/	Quick Look
615	73P/SW3	18.2084	-9.2837	17.581929	-9.54866	13.13101	-15.70655	139.744498	-71.45365551	59.3985	53894.2087384259	2006-06-08 05:00:35	53894.2689467593	2006-06-08 06:27:17	500014090	1.5089	35	1.5089	1.5089	1.5089	1.5089	1	1	1	1	1	0	0	1.6552	1.6552	5.202	0	PROCESSED	57534.5937037037	2016-05-26 14:14:56	54267	2007-06-16 00:00:00	54052.5382986111	2006-11-13 12:55:09	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014090/	Quick Look
616	CYGNUS LOOP NE1	314.1885	31.738	313.671289	31.544868	329.414773	46.489683	75.60815027	-8.84073861	223.0005	53697.7354282407	2005-11-23 17:39:01	53698.2051388889	2005-11-24 04:55:24	500020010	20.3437	20	20.3517	20.3517	20.3517	20.3437	1	1	1	1	1	0	0	17.992	17.992	40.5759	0	PROCESSED	57528.0684837963	2016-05-20 01:38:37	54247	2007-05-27 00:00:00	54037.9167476852	2006-10-29 22:00:07	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001093	We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	0	SWG	CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500020010/	Quick Look
617	CYGNUS LOOP NE2	313.9681	31.9542	313.452396	31.761838	329.292075	46.763002	75.65570239	-8.55863001	223.0005	53698.2056134259	2005-11-24 04:56:05	53698.6766666667	2005-11-24 16:14:24	500021010	21.4135	20	21.4455	21.4375	21.4295	21.4135	2	2	2	2	1	0	0	21.6541	21.6541	40.6939	0	PROCESSED	57528.0693518518	2016-05-20 01:39:52	54247	2007-05-27 00:00:00	54038.4014351852	2006-10-30 09:38:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001093	We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	0	SWG	CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500021010/	Quick Look
618	GALACTIC CENTER GC2	265.779	-29.1853	264.9833	-29.162875	266.287161	-5.798531	359.50136289	0.33591697	108.7998	54170.1638773148	2007-03-11 03:55:59	54170.7946064815	2007-03-11 19:04:14	501047010	25.599	25	25.607	25.599	0	25.623	1	1	0	1	1	0	0	19.0886	19.0886	54.4799	0	PROCESSED	57537.6398611111	2016-05-29 15:21:24	54736	2008-09-27 00:00:00	54182.2693865741	2007-03-23 06:27:55	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501047010/	Quick Look
619	HIGH LAT. DIFFUSE B	38.7468	-52.2774	38.331334	-52.495237	4.39034	-61.411521	272.40280946	-58.27300774	280.6379	53783.933900463	2006-02-17 22:24:49	53786.5211111111	2006-02-20 12:30:24	500027020	103.553	100	103.553	103.561	103.561	103.561	2	2	2	2	1	0	0	68.6094	68.6094	223.5238	3	PROCESSED	57533.0790972222	2016-05-25 01:53:54	54247	2007-05-27 00:00:00	54041.5670717593	2006-11-02 13:36:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000044	We propose observing the diffse background at two locations where the low temperature component is particularly string. One of the these enhancement is ostensibly an extension of the local bubble, while the other it is probably due to a region of very bright emission in the halo (z> 400 pc). We can verify the thermal nature of these sources, and look for CNO abyndance ratio differences between local disk and halo gas. It is critical to make these abundance determinations before the low energy response deteriorates any further. Note that this observation should also allow a calibration of the XIS response below the carbon edge to ~20%.	GALACTIC DIFFUSE EMISSION	5	A	SWG		JAP	0	SWG	HIGH LATTITUDE DIFFUSE A & B	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500027020/	Quick Look
620	LMC X-3 OFF FIELD 1	85.5246	-64.555	85.467763	-64.576889	45.273362	-87.277293	274.10794908	-31.71433471	145.4977	54039.3159722222	2006-10-31 07:35:00	54039.7509722222	2006-10-31 18:01:24	501097020	15.3749	10	15.3749	15.3829	15.3829	15.3829	2	2	2	2	1	0	0	14.9263	14.9263	37.58	0	PROCESSED	57536.0002314815	2016-05-28 00:00:20	54526	2008-03-01 00:00:00	54088.8072222222	2006-12-19 19:22:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011256	The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona.	GALACTIC DIFFUSE EMISSION	5	A	Q. DANIEL WANG		USA	1	AO1	A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501097020/	Quick Look
621	GC14	267.1584	-29.141	266.362704	-29.125263	267.496319	-5.724596	0.16624555	-0.66947426	260.5381	54382.6950694444	2007-10-09 16:40:54	54383.1530555556	2007-10-10 03:40:24	502002010	23.1903	20	23.2063	23.1903	0	23.2063	1	1	0	1	1	0	0	20.9329	20.9329	39.5599	0	PROCESSED	57540.2209490741	2016-06-01 05:18:10	54771	2008-11-01 00:00:00	54402.7240740741	2007-10-29 17:22:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502002010/	Quick Look
622	COMET_8P_TUTTLE-P2_18	40.6547	-37.9803	40.155519	-38.192358	20.729743	-50.258243	244.9394556	-64.31314542	254.1595	54492.2963773148	2008-01-27 07:06:47	54492.4293287037	2008-01-27 10:18:14	502063180	6.1505	6	6.1505	6.1505	0	6.1505	1	1	0	1	1	0	0	6.6133	6.6133	11.4799	0	PROCESSED	57541.4227083333	2016-06-02 10:08:42	54912	2009-03-22 00:00:00	54546.2369675926	2008-03-21 05:41:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063180/	Quick Look
623	ARC2	39.9365	-39.101	39.440937	-39.3153	19.107499	-50.973986	247.81076012	-64.49485898	35.5401	54256.3120486111	2007-06-05 07:29:21	54258.149525463	2007-06-07 03:35:19	502071010	105.7271	100	105.7351	105.7351	0	105.7271	2	2	0	2	1	0	0	82.9236	82.9236	158.7418	1	PROCESSED	57538.8944097222	2016-05-30 21:27:57	54702	2008-08-24 00:00:00	54264.533275463	2007-06-13 12:47:55	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021222	Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants.	GALACTIC DIFFUSE EMISSION	5	B	ROBIN SHELTON		USA	2	AO2	A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502071010/	Quick Look
624	GC_LARGEPROJECT8	265.1842	-30.7499	264.378561	-30.724571	265.818402	-7.37856	357.90048261	-0.05223369	268.8911	54727.1991782407	2008-09-18 04:46:49	54728.3141203704	2008-09-19 07:32:20	503014010	55.3651	50	55.3651	55.3891	0	55.3651	2	2	0	2	1	0	0	51.2069	51.2069	96.3118	1	PROCESSED	57543.8756481482	2016-06-04 21:00:56	54557	2008-04-01 00:00:00	54783.7018055556	2008-11-13 16:50:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503014010/	Quick Look
625	CYGNUS LOOP (P22)	312.8353	32.4047	312.324184	32.216345	328.267069	47.560901	75.39493092	-7.53123997	61.4354	54620.2981134259	2008-06-03 07:09:17	54620.7522453704	2008-06-03 18:03:14	503058010	19.2873	15	19.2873	19.2873	0	19.2873	2	2	0	2	1	0	0	17.2203	17.2203	39.212	0	PROCESSED	57542.7062037037	2016-06-03 16:56:56	55003	2009-06-21 00:00:00	54636.2807638889	2008-06-19 06:44:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503058010/	Quick Look
626	VELA FRAGMENT E	119.9016	-44.3755	119.497107	-44.237549	140.837519	-62.635644	259.34445053	-7.61175769	281.1138	54582.309224537	2008-04-26 07:25:17	54583.7849421296	2008-04-27 18:50:19	503096010	79.2004	70	79.2189	79.2004	0	79.2324	2	2	0	2	1	0	0	84.2529	84.2529	127.4899	1	PROCESSED	57542.4144212963	2016-06-03 09:56:46	54960	2009-05-09 00:00:00	54594.2098842593	2008-05-08 05:02:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031212	Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM.	GALACTIC DIFFUSE EMISSION	5	B	TERRANCE GAETZ		USA	3	AO3	SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503096010/	Quick Look
627	BLOWOUT5	312.2204	31.3402	311.705242	31.154062	326.94204	46.789679	74.2273165	-7.78955911	225.5762	55176.0660532407	2009-12-11 01:35:07	55176.7307175926	2009-12-11 17:32:14	504015010	30.4064	25	30.4064	30.4064	0	30.4064	2	2	0	2	1	0	0	28.6921	28.6921	57.4239	0	PROCESSED	57549.7666898148	2016-06-10 18:24:02	55555	2010-12-25 00:00:00	55189.2693981482	2009-12-24 06:27:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504015010/	Quick Look
628	NGC 6888	303.111	38.3992	302.65502	38.248061	320.307714	56.205556	75.54872423	2.39562358	36.3096	54999.0718981482	2009-06-17 01:43:32	55001.1793287037	2009-06-19 04:18:14	504084010	88.8468	75	88.8548	88.8468	0	88.8548	2	2	0	2	1	0	0	82.4052	82.4052	182.0679	2	PROCESSED	57547.6754976852	2016-06-08 16:12:43	55378	2010-07-01 00:00:00	55012.4221180556	2009-06-30 10:07:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041321	Fast winds from massive stars create large cavities in the surrounding interstellar medium filled with hot gas, known as Wind-Blown Bubbles (WBB). We propose to obtain XIS imaging spectroscopy of the prototype WBB NGC 6888. Thanks to the XIS excellent sensitivity and energy resolution in the soft X-ray band, we will: (i) obtain a high quality CCD spectrum which can be used to constrain the temperature of the hot plasma and the efficiency of thermal conduction across the bubble wall, (ii) determine the spatial distribution and properties of X-ray emitting plasma, (iii) therefore, test and refine shock physics models of bubbles by a direct confrontation of their results with observations.	GALACTIC DIFFUSE EMISSION	5	A	SVETOZAR ZHEKOV		USA	4	AO4	X-RAYS FROM THE PROTOTYPE WIND-BLOWN BUBBLE NGC 6888	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504084010/	Quick Look
629	CYGNUS LOOP 9	312.876	30.2229	312.354142	30.034417	327.064975	45.541284	73.70000859	-8.9268412	80.5836	55307.2796064815	2010-04-21 06:42:38	55308.0106597222	2010-04-22 00:15:21	505017010	29.9968	29	29.9968	29.9968	0	29.9968	2	2	0	2	1	0	0	27.6281	27.6281	63.1499	1	PROCESSED	57551.2933217593	2016-06-12 07:02:23	55287	2010-04-01 00:00:00	55364.2675347222	2010-06-17 06:25:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505017010/	Quick Look
630	SNR G304.6+0.1	196.4463	-62.6951	195.657347	-62.427468	227.041423	-49.777353	304.57643925	0.13082789	321.0575	55442.9126736111	2010-09-03 21:54:15	55445.5356828704	2010-09-06 12:51:23	505074010	99.5817	100	99.6217	99.5817	0	99.6297	2	2	0	2	1	0	0	90.5653	90.5653	226.5319	1	PROCESSED	57553.3505555556	2016-06-14 08:24:48	55827	2011-09-23 00:00:00	55461.4231712963	2010-09-22 10:09:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051306	Galactic supernova remnants are believed to be the primary source of cosmic rays below 10^15.5 eV even though the exact acceleration mechanism remains unknown. This uncertainty results from the lack of remnants with synchrotron X-ray and GeV emission, needed to distinguish accelerated electrons from protons using broadband spectral modeling. An analysis of recent XMM and Fermi data suggests SNR G304.6+0.1 is just the third remnant with both, but the observed hard X-ray excess is also consistent with bremsstrahlung emission. We request a deep Suzaku observation of this source to determine the nature of its hard X-ray emission - critical for identifying the underlying acceleration mechanism.	GALACTIC DIFFUSE EMISSION	5	B	JOSEPH GELFAND		USA	5	AO5	THE ORIGIN OF THE HARD X-RAY AND GEV GAMMA-RAY EMISSION OF SNR G304.6+0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505074010/	Quick Look
631	GALACTIC_BULGE6	271.3758	-31.4828	270.564538	-31.487512	271.175264	-8.047458	359.95693453	-4.99276165	88.0304	55639.361087963	2011-03-19 08:39:58	55640.3565162037	2011-03-20 08:33:23	505081010	50.1669	50	50.1714	50.1669	0	50.1795	3	2	0	2	1	0	0	43.6357	43.6357	85.9898	0	PROCESSED	57601.2415277778	2016-08-01 05:47:48	55287	2010-04-01 00:00:00	55649.2186574074	2011-03-29 05:14:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505081010/	Quick Look
632	GALACTIC_BULGE14	264.9946	-32.433	264.177795	-32.406725	265.713815	-9.066176	356.38820164	-0.80858885	270.5244	55479.5865509259	2010-10-10 14:04:38	55480.8980671296	2010-10-11 21:33:13	505083010	52.9383	50	52.9383	52.9383	0	52.9383	1	1	0	1	1	0	0	42.4073	42.4073	113.3039	1	PROCESSED	57553.7064236111	2016-06-14 16:57:15	55287	2010-04-01 00:00:00	55491.0402893518	2010-10-22 00:58:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505083010/	Quick Look
633	THE KEPLER SNR	262.6745	-21.5044	261.925136	-21.467093	263.174286	1.76325	4.50818409	6.8092486	272.4561	55469.9826736111	2010-09-30 23:35:03	55470.368287037	2010-10-01 08:50:20	505092010	17.7141	620	17.7221	17.7301	0	17.7141	2	2	0	2	1	0	0	17.8694	17.8694	33.3079	0	PROCESSED	57553.595	2016-06-14 14:16:48	55287	2010-04-01 00:00:00	55482.4747453704	2010-10-13 11:23:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092010/	Quick Look
634	3C 59 VICINITY 1	32.0992	30.0806	31.374147	29.84386	40.280714	16.078754	142.1363254	-29.90513458	254.1341	55940.8410763889	2012-01-14 20:11:09	55942.215474537	2012-01-16 05:10:17	506024010	55.8581	50	55.8581	55.8581	0	55.8581	2	2	0	2	1	0	0	46.0404	46.0404	118.7379	1	PROCESSED	57604.3853356482	2016-08-04 09:14:53	56331	2013-02-08 00:00:00	55960.1998032407	2012-02-03 04:47:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060067	We propose for an observation of the vicinities of 3C 59, in order to study the radial extent of the Galactic hot gas. We have conducted joint analysis of absorption and emission lines toward several targets until now and successfully constrained the temperature, line-of-sight length, and density of the hot gas of the directions. However, all the line-of-sight lengths of the hot gas for the past surveys stay within the Galactic disc with the radius of 10 kpc, therefore the radial extent of the gas is still unknown. Emission analysis of low-latitude and almost anti-center directed 3C 59 will constrain the extent, and the result will be unambiguous when emission and absorption lines are jointly analyzed.	GALACTIC DIFFUSE EMISSION	5	C	KAZUHIRO SAKAI		JAP	6	AO6	STUDY OF RADIAL DISTRIBUTION OF THE HOT INTERSTELLAR MEDIUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506024010/	Quick Look
635	G18.8+0.3	275.9435	-12.3781	275.241856	-12.405238	275.902948	10.940788	18.78460262	0.39706413	83.4994	55994.9180324074	2012-03-08 22:01:58	55996.1598958333	2012-03-10 03:50:15	506051010	52.0205	50	52.0205	52.0285	0	52.0365	2	2	0	2	1	0	0	44.882	44.882	107.2639	1	PROCESSED	57604.8541435185	2016-08-04 20:29:58	56382	2013-03-31 00:00:00	56016.6717708333	2012-03-30 16:07:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061311	We propose a 50 ks exploratory observation of an interesting first-quadrant supernova remnant, G18.8+0.3, for which radio-continuum and CO data indicate interaction with a molecular cloud. Prior X-ray studies are limited to a 14 ks ROSAT PSPC observation producing about 500 counts. We expect about 12,000 counts with Suzaku, which should permit basic characterization of the spectrum and morphology of X-rays: shell-type, mixed-morphology (central thermal emission) or even composite (central PWN). Spectral analysis will allow us to determine or estimate shock speed, age, ambient density, and swept-up mass. As more middle-aged remnants are found to have unusual properties such as GeV-TeV emission, the study of objects like G18.8+0.3 assumes greater importance.	GALACTIC DIFFUSE EMISSION	5	C	STEPHEN REYNOLDS		USA	6	AO6	G18.8+0.3: A SUPERNOVA REMNANT WITH STRONG MOLECULAR INTERACTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506051010/	Quick Look
636	G272.2-3.2	136.7114	-52.1231	136.316281	-51.921066	170.818449	-63.077248	272.22308022	-3.18374401	297.1287	55709.5476041667	2011-05-28 13:08:33	55711.9009490741	2011-05-30 21:37:22	506060010	130.0782	150	130.0862	130.0942	0	130.0782	2	2	0	2	1	0	0	121.8303	121.8303	203.3058	3	PROCESSED	57602.216087963	2016-08-02 05:11:10	55652	2011-04-01 00:00:00	55735.3493171296	2011-06-23 08:23:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506060010/	Quick Look
637	HESSJ1507-622_CENTER	226.7316	-62.3464	225.708755	-62.153708	244.337801	-42.703137	317.95199358	-3.49348671	301.8082	56181.4881712963	2012-09-11 11:42:58	56183.9549189815	2012-09-13 22:55:05	507025010	79.8869	80	79.8949	79.9029	0	79.8869	2	2	0	2	1	0	0	74.1958	74.1958	213.1037	1	PROCESSED	57607.0557986111	2016-08-07 01:20:21	56582	2013-10-17 00:00:00	56212.7347337963	2012-10-12 17:38:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070033	HESS J1507-622 is one of the unidentified TeV-gamma-ray sources discovered in the H.E.S.S. Galactic plane survey. The object is unique in the sense of the location, off the Galactic plane. There are no counterparts in radio, infrared, X-ray bands and thus the origin is still mystery, but the object represents several hints; X-ray source like pulsar wind nebula exists near the object, and the location is at the edge of the large molecular cloud near a radio supernova remnant. The main purpose of the Suzaku observation with the best use of high sensitive capability in diffuse X-rays and of a unique low galactic-absorption feature of the object is to determine the origin of TeV emission, such as old supernova remnant with molecular cloud, pulsar-wind driven radiations, or darkest accelerator.	GALACTIC DIFFUSE EMISSION	5	B	YUKIKATSU TERADA	HIRONORI MATSUMOTO	JAP	7	AO7	SUZAKU OBSERVATION OF HESS J1507-622; A UNIQUE TEV UNIDENTIFIED SOURCE OFF THE GALACTIC PLANE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507025010/	Quick Look
638	CAS A	350.8607	58.8031	350.294827	58.528522	27.373119	54.842451	111.73599633	-2.14263527	251.3043	56281.1375115741	2012-12-20 03:18:01	56283.3466666667	2012-12-22 08:19:12	507038010	102.411	100	102.419	102.411	0	102.426	2	1	0	2	1	0	0	126.7103	126.7103	190.8458	0	PROCESSED	57608.4566435185	2016-08-08 10:57:34	56683	2014-01-26 00:00:00	56316.9831365741	2013-01-24 23:35:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070050	We will propose a follow-up 120 ksec observations of a young supernova remnant Cassiopeia A. The long exposure provides us a high quality of the broad band spectrum from XIS to HXD GSO band. We will try to detect Mn-K line at 6.1 keV for the first time. The element Mn as well as Cr gives constraint on the explosion mechanism of the ejecta. We also test a predicted flux variation of a non-thermal emission in the PIN band for the first time. The variation gives critical information to solve the physical parameters in the reverse shock of the ejecta.	GALACTIC DIFFUSE EMISSION	5	C	YOSHITOMO MAEDA		JAP	7	AO7	MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507038010/	Quick Look
639	GRXE_E_5	268.0495	-26.6011	267.269457	-26.589728	268.243808	-3.171982	2.75089625	-0.04390767	105.4995	56373.3059722222	2013-03-22 07:20:36	56375.3646990741	2013-03-24 08:45:10	507072010	101.2435	100	101.2435	101.2435	0	101.2435	2	2	0	2	1	0	0	102.6676	102.6676	177.8658	1	PROCESSED	57610.9241087963	2016-08-10 22:10:43	56018	2012-04-01 00:00:00	56384.595787037	2013-04-02 14:17:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507072010/	Quick Look
640	W28_SOUTH	270.2522	-23.558	269.490042	-23.557374	270.221597	-0.117322	6.38418356	-0.23955939	89.9033	56738.9940393518	2014-03-22 23:51:25	56740.1793518518	2014-03-24 04:18:16	508006010	40.8518	100	40.8838	40.8518	0	40.8942	1	1	0	2	1	0	0	35.4568	35.4568	102.4078	1	PROCESSED	57614.1110648148	2016-08-14 02:39:56	57359	2015-12-03 00:00:00	56754.6877083333	2014-04-07 16:30:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080017	A series of discoveries of recombining plasma (RP) in mixed-morphology (MM) SNRs inspires us with a new scenario for SNR evolution. The observed spectra are well described by the picture that the plasma has experienced sudden cooling in the past and currently undergoes gradual recombination to ionization equilibrium. In the MM SNR W28, we found the spatial correlation between the radio brightness and the thermal evolution (recombination) phase. Hence, the radio-fainter region may have less recombined plasma. Such a plasma should emit strong Fe-K line from the He-like ions. The line flux reflects the initial temperature of RP, which brings the key information of the explosion environment of MM SNRs. For this purpose, we propose a 100-ks observation of W28 south, the possible 'youngest' RP.	GALACTIC DIFFUSE EMISSION	5	A	MAKOTO SAWADA		JAP	8	AO8	INITIAL PARAMETERS OF RECOMBINING PLASMA IN SUPERNOVA REMNANTS EXPLORED THROUGH W28	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508006010/	Quick Look
641	CYG_COCOON2	306.1992	40.9463	305.753337	40.782769	326.198572	57.540222	78.99355785	1.86268914	253.1744	56603.8842939815	2013-11-07 21:13:23	56605.000162037	2013-11-09 00:00:14	508020010	46.4489	50	46.4489	46.4489	0	46.4489	2	2	0	2	1	0	0	44.6569	44.6569	96.3739	3	PROCESSED	57613.2763194444	2016-08-13 06:37:54	57018	2014-12-27 00:00:00	56652.6462152778	2013-12-26 15:30:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080048	The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density and spatial distribution in this important object.	GALACTIC DIFFUSE EMISSION	5	C	TSUNEFUMI MIZUNO		JAP	8	AO8	SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508020010/	Quick Look
642	VELA PWN W4	126.476	-45.2086	126.060911	-45.04388	150.453491	-61.215385	262.5995548	-4.15230559	95.0003	56591.4348726852	2013-10-26 10:26:13	56591.8813888889	2013-10-26 21:09:12	508045010	16.8588	15	16.8843	16.8588	0	16.8748	2	2	0	2	1	0	0	16.0055	16.0055	38.578	0	PROCESSED	57613.1152893518	2016-08-13 02:46:01	57009	2014-12-18 00:00:00	56643.6542708333	2013-12-17 15:42:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080090	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered.	GALACTIC DIFFUSE EMISSION	5	B	KOJI MORI		JAP	8	AO8	SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508045010/	Quick Look
643	VELA PWN GEV6	128.0698	-45.8067	127.654656	-45.635799	153.081718	-61.174639	263.73946045	-3.59392918	121.6832	56987.9020717593	2014-11-26 21:38:59	56988.5530324074	2014-11-27 13:16:22	509016010	18.0926	15	18.1086	18.0926	0	18.1086	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.8287037037	2016-08-16 19:53:20	57450	2016-03-03 00:00:00	57083.4111574074	2015-03-02 09:52:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090046	We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	9	AO9	X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509016010/	Quick Look
644	L106_B3	337.3111	61.2453	336.866796	60.988922	21.907924	61.425064	106.66847152	2.94694679	86.3781	55332.0617013889	2010-05-16 01:28:51	55333.5078587963	2010-05-17 12:11:19	505054010	59.3804	60	59.3804	59.3804	0	59.3804	3	2	0	2	1	0	0	54.0551	54.0551	124.908	3	PROCESSED	57551.5609259259	2016-06-12 13:27:44	55765	2011-07-23 00:00:00	55393.2646759259	2010-07-16 06:21:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050086	We propose observarions of two fields on and near midplane (b = 0 and 3 deg.) in order to study bump-like emission peaked at 0.9 keV observed in midplane. The two fields proposed for observations has been observed by Chandra. By comparing the spectra taken by Suzaku and Chandra, we will determine the contribution of point sources (stars), and investigate posisble contribution of diffuse thermal plasma.	GALACTIC DIFFUSE EMISSION	5	B	YOH TAKEI		JAP	5	AO5	ORIGIN OF SOFT X-RAY EMISSION IN THE MILKY-WAY DISK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505054010/	Quick Look
645	VICINITY_4U1957+11	300.5977	12.1307	300.008296	11.990222	305.849194	31.842544	52.0534723	-9.74567764	252.1551	55499.6275578704	2010-10-30 15:03:41	55501.8265625	2010-11-01 19:50:15	505057010	80.5839	80	80.5839	80.5839	0	80.5839	2	2	0	2	1	0	0	59.2042	59.2042	189.9759	2	PROCESSED	57553.9949305556	2016-06-14 23:52:42	55882	2011-11-17 00:00:00	55515.3752083333	2010-11-15 09:00:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050090	We propose for an observation of the vicinity of 4U 1957+11, in order to study the Galactic low-latitude hot gas. Recently, detection of OVII and NeIX aborption lines was reported in the spectrum of 4U 1957+11 (Yao et al. 2008). By combining a Suzaku observation of diffuse hot plasma around the object with the reported absorption line equivalnet widths, we will constrain the temperature, line-of-sight length, density of the hot plasma of the direction. Not only to understand the Galactic gas, but also to understand feedback mechanism from a galaxy to the intergalactic space will our study play an important role.	GALACTIC DIFFUSE EMISSION	5	B	YOH TAKEI		JAP	5	AO5	EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC LOW-LATITUDE HOT GAS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505057010/	Quick Look
646	RCW86 SW	220.2761	-62.6782	219.292066	-62.464185	240.754321	-44.190898	315.14426109	-2.43598628	109.6929	53778.0961689815	2006-02-12 02:18:29	53780.2814699074	2006-02-14 06:45:19	500004010	100.7659	100	100.7819	100.7659	100.7819	100.7819	2	2	2	2	1	0	0	90.6819	90.6819	188.7918	2	PROCESSED	57533.035787037	2016-05-25 00:51:32	54247	2007-05-27 00:00:00	54041.2835648148	2006-11-02 06:48:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001019	The supernova remnants (SNRs) are most convincing candidates for the acceleration of cosmic-rays. Together with the TeV gamma-ray detection by CANGAROO and HESS, it is now confirmed that at least some of the SNRs can actually accelerate electrons up to > 10 TeV. However, such studies have not provided direct information on ``protons'', which is the major component of cosmic-rays. Here we propose to measure spatial distribution of accelerated protons in the shell of RCW 86, and its association with the high energy (>10 TeV) electrons which emit synchrotron X-rays up to 50 keV. Large effective area and the good detection capability of Suzaku will be ideal tools for our scientific goal.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	0	SWG	THE FIRST DIRECT MAPPING OF ACCELERATED PROTONS IN THE SW SHELL OF RCW 86	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500004010/	Quick Look
647	73P/SW3	279.2884	33.5067	278.829487	33.462856	284.096243	56.493773	62.26395264	17.33399104	47.3721	53862.3946875	2006-05-07 09:28:21	53862.4794444444	2006-05-07 11:30:24	500012010	3.25	5	3.25	3.25	3.25	3.25	1	1	1	1	1	0	0	2.3139	2.3139	7.304	0	PROCESSED	57533.6418402778	2016-05-25 15:24:15	54256	2007-06-05 00:00:00	54042.1755671296	2006-11-03 04:12:49	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500012010/	Quick Look
648	JUPITER	29.0829	10.6504	28.417372	10.406323	30.788902	-1.172897	147.71201597	-49.07381266	249.1851	55939.2483912037	2012-01-13 05:57:41	55939.8634722222	2012-01-13 20:43:24	506006050	23.2827	160	23.2907	23.2827	0	23.2954	2	2	0	2	1	0	0	19.2679	19.2679	53.136	0	PROCESSED	57604.3330902778	2016-08-04 07:59:39	56331	2013-02-08 00:00:00	55960.1390740741	2012-02-03 03:20:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060017	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter.	GALACTIC DIFFUSE EMISSION	5	B	KUMI ISHIKAWA		JAP	6	AO6	STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006050/	Quick Look
649	WESTERLUND1_2	252.808	-46.1402	251.891543	-46.055758	257.089266	-23.465452	339.79276992	-1.14410237	285.6981	55451.2033912037	2010-09-12 04:52:53	55452.6077777778	2010-09-13 14:35:12	505050010	52.6541	50	52.6541	52.6541	0	52.6541	2	2	0	2	1	0	0	42.7536	42.7536	121.3099	0	PROCESSED	57553.3934375	2016-06-14 09:26:33	55829	2011-09-25 00:00:00	55463.2091435185	2010-09-24 05:01:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050078	TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster.	GALACTIC DIFFUSE EMISSION	5	A	HIRONORI MATSUMOTO		JAP	5	AO5	IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505050010/	Quick Look
650	SNR G106.3+2.7 P2	336.9121	60.9439	336.468568	60.688281	21.166616	61.378787	106.34649405	2.79001657	12.2687	55423.4230787037	2010-08-15 10:09:14	55424.0209837963	2010-08-16 00:30:13	505072010	24.5562	50	24.5722	24.5562	0	24.5722	1	1	0	1	1	0	0	26.6147	26.6147	51.6559	1	PROCESSED	57553.084212963	2016-06-14 02:01:16	55807	2011-09-03 00:00:00	55441.2685069444	2010-09-02 06:26:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051305	After two decades searching for the origin of the GeV emission from 3EG J2227+6122, it is now identified with PSR J2229+6114 and its PWN.~This highly energetic young pulsar lies within the arcmin diameter Boomerang radio nebula. Now, recently discovered nearby extended TeV emission suggest a second Vela-like "cocoon" feed by relic electrons from the PWN, blowing out the vast degree-scale radio feature.~Interactions of the SNR shock front with overlapping molecular cloud material can also contribute in the gamma-ray production.~An XIS mosaic will allow us to search for soft and hard X-ray emission similar to Vela's "Cocoon" and resolve the nature of the TeV emission and its connection to the Boomerang and the radio feature.	GALACTIC DIFFUSE EMISSION	5	C	ESTER ALIU		USA	5	AO5	ORIGIN OF THE VHE GAMMA-RAY EMISSION FROM SNR G106.3+2.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505072010/	Quick Look
651	CARINA SW	160.2531	-60.104	159.777159	-59.842292	202.080754	-59.579426	287.34811018	-1.23919183	109.6766	55542.7308333333	2010-12-12 17:32:24	55543.4438888889	2010-12-13 10:39:12	505075010	47.0039	45	47.0039	47.0119	0	47.0119	1	1	0	1	1	0	0	42.4341	42.4341	61.5999	0	PROCESSED	57554.3916435185	2016-06-15 09:23:58	55960	2012-02-03 00:00:00	55592.9230324074	2011-01-31 22:09:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051312	X-ray nebulae with kT =0.1-0.8 keV, log Lx up to 35 ergs/s, and size of 1-1000 pc accompany a number of giant HII region. The Carinae Nebula is the best region to study their origin with 10-100 times more luminous soft X-rays than any other giant HII regions in our Galaxy. X-ray observations especially with Suzaku revealed that a part, or all, of the diffuse plasma would heat up by earlier supernova explosions, but it is unknown when these explosions occurred and how they made the current X-ray nebula. The Chandra Carina Complex Project displayed that the southern part of the nebula emits strong hydrogen-like oxygen line. We will measure helium-like oxygen line with Suzaku to measure its plasma temperature and abundance to help understand relation with plasma in the nebula center.	GALACTIC DIFFUSE EMISSION	5	C	KENJI HAMAGUCHI		USA	5	AO5	SOUTHERN PART OF DIFFUSE PLASMA IN THE CARINA NEBULA - RICH IN OXYGEN?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505075010/	Quick Look
652	CYGNUS LOOP BLOWOUT5	312.5999	28.7931	312.071808	28.605616	325.981178	44.311018	72.41540255	-9.63024021	60.972	55708.6627546296	2011-05-27 15:54:22	55709.5335185185	2011-05-28 12:48:16	506015010	36.7552	35	36.7632	36.7552	0	36.7695	3	2	0	2	1	0	0	31.6317	31.6317	75.216	1	PROCESSED	57602.1728935185	2016-08-02 04:08:58	56093	2012-06-15 00:00:00	55725.2447569444	2011-06-13 05:52:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060053	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	6	AO6	MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506015010/	Quick Look
653	THE KEPLER SNR	262.6706	-21.4823	261.92136	-21.444974	263.169538	1.785137	4.52493262	6.82424916	102.5027	55615.8474421296	2011-02-23 20:20:19	55616.8174768518	2011-02-24 19:37:10	505092030	34.2015	150	34.2095	34.2015	0	34.2095	2	2	0	2	1	0	0	29.1199	29.1199	83.7958	0	PROCESSED	57601.0436342593	2016-08-01 01:02:50	55287	2010-04-01 00:00:00	55628.1747569444	2011-03-08 04:11:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092030/	Quick Look
654	VELA JR SE2	133.8563	-47.0644	133.431556	-46.872219	161.338969	-60.118086	267.19687484	-1.23927515	109.9991	56620.734375	2013-11-24 17:37:30	56621.062650463	2013-11-25 01:30:13	508061010	14.4492	15	14.4492	14.4711	0	14.4572	1	1	0	1	1	0	0	18.7997	18.7997	28.3599	0	PROCESSED	57613.398912037	2016-08-13 09:34:26	56998	2014-12-07 00:00:00	56632.5722685185	2013-12-06 13:44:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080117	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr.	GALACTIC DIFFUSE EMISSION	5	C	TARO FUKUYAMA		JAP	8	AO8	OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR.	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508061010/	Quick Look
655	VELA PWN E4	130.4202	-45.4045	129.99462	-45.224746	155.536956	-59.986634	264.40968594	-2.03918199	304.5026	55712.4105902778	2011-05-31 09:51:15	55712.7362268518	2011-05-31 17:40:10	506047010	17.0314	15	17.0354	17.0549	0	17.0314	2	2	0	2	1	0	0	15.1078	15.1078	28.128	0	PROCESSED	57602.173900463	2016-08-02 04:10:25	56093	2012-06-15 00:00:00	55726.0290046296	2011-06-14 00:41:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506047010/	Quick Look
656	VELAFRAGG TAIL	125.0448	-47.7009	124.65466	-47.541789	151.337516	-63.864294	264.09848727	-6.37839252	263.1844	55658.0366898148	2011-04-07 00:52:50	55658.8565162037	2011-04-07 20:33:23	506057010	49.3543	50	49.3703	49.3543	0	49.3703	3	2	0	2	1	0	0	43.9581	43.9581	70.8259	1	PROCESSED	57601.4287268518	2016-08-01 10:17:22	56043	2012-04-26 00:00:00	55673.1976736111	2011-04-22 04:44:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062021	The Vela supernova remnant (SNR) displays remarkable features which appear to be ejecta ``shrapnel'' visible beyond the main shell. One of these shrapnel (A) is distinct from the others in that its X-ray spectrum exhibits a high Si abundance, while the other shrapnel exhibit enhanced O, Ne, and Mg abundances. One unexplored ejecta shrapnel (G) is located on the opposite side of the remnant from shrapnel A, suggesting that the SN explosion may have resulted in a jet-counterjet Si-rich structure, reminiscent of Cas A. We propose to observe this shrapnel for the first time to determine if it is also Si-rich like shrapnel A. If this is the case, the Vela SNR may be the first direct evidence of a jet-induced SN explosion.	GALACTIC DIFFUSE EMISSION	5	A	FABRIZIO BOCCHINO		EUR	6	AO6	ASYMMETRIC SN EXPLOSION IN VELA SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506057010/	Quick Look
657	CAS A	350.8704	58.8069	350.304462	58.532314	27.384002	54.841803	111.74200441	-2.14072863	228.5251	56672.9492708333	2014-01-15 22:46:57	56673.8064699074	2014-01-16 19:21:19	508011010	0	120	0	0	0	0	0	0	0	0	0	0	0	0	0	0	0	PROCESSED	57613.771412037	2016-08-13 18:30:50	56717	2014-03-01 00:00:00	56712.601400463	2014-02-24 14:26:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080021	We will propose a follow-up 120 ksec observations of a young supernova remnant Cassiopeia A. The long exposure provides us a high quality of the broad band spectrum from XIS to HXD GSO band. We will try to detect Mn-K line at 6.1 keV for the first time. The element Mn as well as Cr gives constraint on the explosion mechanism of the ejecta. We also test a predicted flux variation of a non-thermal emission in the PIN band for the first time. The variation gives critical information to solve the physical parameters in the reverse shock of the ejecta.	GALACTIC DIFFUSE EMISSION	5	B	YOSHITOMO MAEDA		JAP	8	AO8	MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508011010/	Quick Look
658	W44_SOUTH	284.0546	1.2208	283.419443	1.15468	285.391807	23.913502	34.56340933	-0.50670684	73.0006	56756.507025463	2014-04-09 12:10:07	56757.3474074074	2014-04-10 08:20:16	508003020	32.3696	33	32.3776	32.3776	0	32.3696	3	2	0	2	1	0	0	29.5034	29.5034	72.5959	1	PROCESSED	57614.2259837963	2016-08-14 05:25:25	57193	2015-06-20 00:00:00	56825.6834027778	2014-06-17 16:24:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080012	W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	8	AO8	MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508003020/	Quick Look
659	N63A	83.9019	-66.0368	83.884731	-66.066447	9.218584	-87.500527	275.90835505	-32.28360929	166.1398	56628.8025347222	2013-12-02 19:15:39	56629.9556828704	2013-12-03 22:56:11	508071010	82.0387	80	82.0467	82.0387	0	82.0467	2	2	0	2	1	0	0	70.8129	70.8129	99.6119	3	PROCESSED	57613.5008680556	2016-08-13 12:01:15	56383	2013-04-01 00:00:00	56639.6281365741	2013-12-13 15:04:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081315	We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		USA	8	AO8	LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508071010/	Quick Look
660	MBM16	49.7645	11.5821	49.080902	11.401011	50.440387	-6.505796	170.59989958	-37.2737153	77.5997	56511.9409027778	2013-08-07 22:34:54	56513.916875	2013-08-09 22:00:18	508078010	82.3246	80	82.3246	82.3246	0	82.3246	2	2	0	2	1	0	0	79.0718	79.0718	170.6898	2	PROCESSED	57612.2763541667	2016-08-12 06:37:57	56383	2013-04-01 00:00:00	56587.6759490741	2013-10-22 16:13:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086002	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	8	AO8	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508078010/	Quick Look
661	MBM36	238.3853	-4.8926	237.724645	-4.745297	237.254427	15.02643	3.92555744	35.61619893	279.5456	56531.6987268518	2013-08-27 16:46:10	56533.8883333333	2013-08-29 21:19:12	508079020	79.6067	80	79.6067	79.6067	0	79.6067	2	2	0	2	1	0	0	67.717	67.717	189.166	2	PROCESSED	57612.4621064815	2016-08-12 11:05:26	56383	2013-04-01 00:00:00	56603.7246875	2013-11-07 17:23:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086002	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	8	AO8	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508079020/	Quick Look
662	G93.3+6.9 SOUTH	313.0658	55.1877	312.717301	54.998248	351.809721	66.81178	93.13746865	6.81993623	52.2984	56817.2417708333	2014-06-09 05:48:09	56819.1057638889	2014-06-11 02:32:18	509041010	85.4695	80	85.7132	85.4695	0	85.7131	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.2181712963	2016-08-15 05:14:10	57201	2015-06-28 00:00:00	56835.7539236111	2014-06-27 18:05:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091316	We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN.	GALACTIC DIFFUSE EMISSION	5	C	MICHAEL STAGE		USA	9	AO9	G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509041010/	Quick Look
663	FERMI_JET_COCOON_1	324.2719	-34.1434	323.519422	-34.36838	315.213492	-18.826861	11.0027102	-48.00136957	252.0162	56980.9718402778	2014-11-19 23:19:27	56981.4029166667	2014-11-20 09:40:12	509047010	23.1647	20	23.1647	23.1887	0	23.1727	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.793125	2016-08-16 19:02:06	57444	2016-02-26 00:00:00	57076.4062037037	2015-02-23 09:44:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091322	The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way.	GALACTIC DIFFUSE EMISSION	5	C	MATTHEW MILLER		USA	9	AO9	OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509047010/	Quick Look
664	DIFFUSE1CENTER	201.5497	7.7363	200.922947	7.99578	196.916148	15.561038	327.54309857	68.93048937	123.2999	57014.2523842593	2014-12-23 06:03:26	57014.7820949074	2014-12-23 18:46:13	509058010	20.5308	20	20.5308	20.5308	0	20.5308	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.5530555556	2016-08-17 13:16:24	57475	2016-03-28 00:00:00	57107.4252546296	2015-03-26 10:12:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091324	In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them.	GALACTIC DIFFUSE EMISSION	5	C	JOEL BREGMAN		USA	9	AO9	UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509058010/	Quick Look
665	3C400.2 NW	294.5044	17.3912	293.942879	17.276968	300.273195	38.29194	53.66788209	-2.01364052	81.5888	56770.4644907407	2014-04-23 11:08:52	56770.9410763889	2014-04-23 22:35:09	509068010	21.47	20	21.4853	21.486	0	21.47	2	2	0	2	1	0	0	20.9678	20.9678	41.1719	0	PROCESSED	57614.9785416667	2016-08-14 23:29:06	57152	2015-05-10 00:00:00	56789.6036805556	2014-05-12 14:29:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092010	Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances.	GALACTIC DIFFUSE EMISSION	5	A	JACCO VINK		EUR	9	AO9	THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509068010/	Quick Look
666	G306.3-0.9	200.4753	-63.5602	199.643661	-63.298602	230.10249	-49.420915	306.31531317	-0.88874973	306.5675	56889.7845833333	2014-08-20 18:49:48	56894.0099768518	2014-08-25 00:14:22	509072010	190.0114	200	190.0181	190.0114	0	190.0114	2	2	0	2	1	0	0	14.4515	14.4515	20.22	0	PROCESSED	57616.5396759259	2016-08-16 12:57:08	57305	2015-10-10 00:00:00	56938.2302777778	2014-10-08 05:31:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	093109	The origin of the distorted, inhomogeneous structure of mixed-morphology SNRs (MM SNRs) is a mystery. Recently we have discovered recombining plasma from MM SNRs. The existence of recombining plasma implies rapid cooling process in past. Recombining plasma, together with the peculiar morphologies, would indicate a new SNR evolution scenario. Our systematic analysis of recombining SNRs shows that the recombination ages are almost the same, although their dynamical ages range over an order of magnitude. Such a trend can be explained by past rapid rarefaction. This hypothesis can be tested by measuring a recombination age of a dynamically young recombining SNR. We thus propose a 100-ks Suzaku observation of G306.3-0.9, a candidate of the youngest recombining SNR ever.	GALACTIC DIFFUSE EMISSION	5	A	MAKOTO SAWADA	Reynolds,Matsumura	JUS	9	AO9	THE DYNAMICS OF MIXED-MORPHOLOGY SNRS PROBED BY THE YOUNGEST RECOMBINING PLASMA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509072010/	Quick Look
667	SN1006_BGD3	226.4731	-42.5186	225.649158	-42.32537	236.222692	-24.044133	327.77356316	13.77561257	286.5156	56888.6466550926	2014-08-19 15:31:11	56889.2084606482	2014-08-20 05:00:11	509085010	31.65	30	31.65	31.65	0	31.65	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5050115741	2016-08-16 12:07:13	56748	2014-04-01 00:00:00	56910.6423611111	2014-09-10 15:25:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096004	We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		USA	9	AO9	THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509085010/	Quick Look
668	CYGNUS_LOOP_P3	313.0409	31.565	312.525205	31.375918	328.010479	46.721185	74.84662265	-8.19493741	240.0003	54418.4174074074	2007-11-14 10:01:04	54418.9377083333	2007-11-14 22:30:18	501014010	16.7648	12	16.7812	16.7808	0	16.7648	2	2	0	2	1	0	0	14.6962	14.6962	44.9439	0	PROCESSED	57540.5210069445	2016-06-01 12:30:15	54798	2008-11-28 00:00:00	54430.2624884259	2007-11-26 06:17:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501014010/	Quick Look
669	SN 1987A	83.8361	-69.2786	83.928024	-69.308301	307.518784	-86.433209	279.71542477	-31.94667609	132.5904	53677.835775463	2005-11-03 20:03:31	53678.3475	2005-11-04 08:20:24	500006010	36.7863	40	36.7863	36.7863	36.7863	36.7863	2	2	2	2	1	0	0	32.9198	32.9198	44.1661	1	PROCESSED	57527.9193518518	2016-05-19 22:03:52	54247	2007-05-27 00:00:00	54037.1281481482	2006-10-29 03:04:32	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001028	SN1987A is providing us with a unique opportunity to study the supernova explosion itself and the very early phase of the supernova-remnants evolution. The supernova blast wave has started to strike the inner circumstellar ring. The neutrino flash observed at the time of explosion implies the formation of a neutron star, but no evidence of this has been detected yet. We propose to observe SN1987A for 40 ksec with Suzaku HXD and XIS. Our first goal is the search for a periodic hard signal from the putative pulsar. We also want to study the collision of the supernova blast wave with the inner ring. In order to follow the temporal evolution of the shock, we propose to observe the source with Suzaku in the early phase of the SWG PV-phase as a reference for further studies.	GALACTIC DIFFUSE EMISSION	5	A	GUENTHER HASINGER		JAP	0	SWG	SUZAKU OBSERVATION OF SN1987A : SEARCH FOR PULSAR EMISSION AND STUDY OF A NEWBORN SNR		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500006010/	Quick Look
670	GALACTIC RIDGE	281.0049	-4.0776	280.344509	-4.129178	281.602156	18.920781	28.45801897	-0.21166151	265.5297	53671.1112037037	2005-10-28 02:40:08	53673.8960069445	2005-10-30 21:30:15	500009010	93.3276	100	93.3436	93.3596	93.3436	93.3276	2	2	2	2	1	0	0	77.5364	77.5364	240.5759	0	PROCESSED	57527.7330439815	2016-05-19 17:35:35	54247	2007-05-27 00:00:00	54037.6929513889	2006-10-29 16:37:51	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001042	We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field.	GALACTIC DIFFUSE EMISSION	5	A	KEN EBISAWA		JAP	0	SWG	ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500009010/	Quick Look
671	73P/SW3	318.3252	23.9905	317.766876	23.78347	329.890581	37.931404	71.97868305	-16.64134569	72.7093	53868.4091666667	2006-05-13 09:49:12	53868.4752199074	2006-05-13 11:24:19	500013050	3.225	20	3.225	3.225	3.225	3.225	1	1	1	1	1	0	0	2.584	2.584	5.7039	0	PROCESSED	57534.2992476852	2016-05-26 07:10:55	54256	2007-06-05 00:00:00	54089.4348611111	2006-12-20 10:26:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013050/	Quick Look
672	73P/SW3	318.7382	23.8104	318.178519	23.602036	330.247137	37.622205	72.09504522	-17.04458663	72.7096	53868.4758333333	2006-05-13 11:25:12	53868.5418865741	2006-05-13 13:00:19	500013060	3.218	20	3.218	3.218	3.218	3.218	1	1	1	1	1	0	0	2.539	2.539	5.6959	0	PROCESSED	57534.3046759259	2016-05-26 07:18:44	54256	2007-06-05 00:00:00	54042.3000462963	2006-11-03 07:12:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013060/	Quick Look
673	73P/SW3	319.575	23.4516	319.012619	23.240566	330.968775	37.00001	72.3420597	-17.8575616	72.7092	53868.609212963	2006-05-13 14:37:16	53868.6738310185	2006-05-13 16:10:19	500013080	3.1644	20	3.1644	3.1644	3.1644	3.1644	1	1	1	1	1	0	0	2.986	2.986	5.5519	0	PROCESSED	57534.3120601852	2016-05-26 07:29:22	54256	2007-06-05 00:00:00	54042.3213657407	2006-11-03 07:42:46	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013080/	Quick Look
674	DRACO HVC REGION A	243.9602	60.0594	243.754378	60.182015	196.928393	76.754112	91.20688798	42.38144862	79.8192	53814.6161111111	2006-03-20 14:47:12	53816.0050578704	2006-03-22 00:07:17	501004010	61.1798	60	61.1798	61.1798	61.1798	61.1798	2	2	2	2	1	0	0	61.2301	61.2301	119.9879	2	PROCESSED	57533.2956481482	2016-05-25 07:05:44	54394	2007-10-21 00:00:00	53906.0459722222	2006-06-20 01:06:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010069	High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	1	AO1	SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE -	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501004010/	Quick Look
675	CAR-D1	162.0244	-59.5887	161.531362	-59.324189	202.52434	-58.576902	287.89332648	-0.36746291	282.973	53891.5567361111	2006-06-05 13:21:42	53892.6343055556	2006-06-06 15:13:24	501099010	76.9074	75	76.924	76.932	76.9314	76.9074	2	2	2	2	1	0	0	64.2576	64.2576	93.0899	0	PROCESSED	57534.5127430556	2016-05-26 12:18:21	54401	2007-10-28 00:00:00	53926.947974537	2006-07-10 22:45:05	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011257	Soft X-ray emission nebulae with kT =0.1-0.8 keV, log Lx =33-35 ergs/s, and the size of 1-1000 pc accompany a number of giant HII region, but the origin is not understood yet. The Carinae Nebula is 10-100 times more luminous than any other giant HII region in our Galaxy in soft X-rays. From an XMM-Newton observation of the eastern tip of the nebula called Car-D1, we found marginal CVI, CV and OVII lines. If it is real, the carbon abundance should be more than >6 solar, and the OVII line requires more than 2-temperature components. To detect those emission lines clearly and address the origin and environment of the diffuse plasma, we propose a Suzaku observation of the Car-D1 region, optimized for the XIS BI chip.	GALACTIC DIFFUSE EMISSION	5	B	KENJI HAMAGUCHI		USA	1	AO1	ORIGIN OF THE DIFFUSE X-RAY EMISSION AROUND THE CARINA NEBULA, A MASSIVE STAR FORMING REGION	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501099010/	Quick Look
676	GALACTIC PLANE 111	347.9369	61.9538	347.407091	61.681886	29.574403	58.088255	111.50111702	1.31488521	81.8498	53892.6499652778	2006-06-06 15:35:57	53893.680775463	2006-06-07 16:20:19	501100010	72.1409	75	72.1649	72.1649	72.1649	72.1409	2	2	2	2	1	0	0	61.025	61.025	89.0349	1	PROCESSED	57534.5221064815	2016-05-26 12:31:50	54401	2007-10-28 00:00:00	53927.3325115741	2006-07-11 07:58:49	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011258	We propose to observe the line of sight towards (l,b)=(111.5,1.3). This line of sight was observed by XMM because the line of sight is particularly simple, allowing the isolation of the spectrum of the Local Hot Bubble (LHB). The XMM observation did not isolate the LHB, but did reveal the existance of a cool (kT~0.18 keV) X-ray emitting component between 200 and 2000 pcs away that was morphologically unidentifiable in the ROSAT All-Sky Survey. This component may represent the gas responsible for the 3/4 keV "infill problem", and may represent a previously overlooked high filling factor component of the hot ISM. Suzaku observations along this line of sight, coupled with the Suzaku observation towards MBM12, will allow the isolation of this component.	GALACTIC DIFFUSE EMISSION	5	B	K. KUNTZ		USA	1	AO1	BEYOND THE LOCAL HOT BUBBLE TOWARDS L=111	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501100010/	Quick Look
677	DRACO ENHANCEMENT	239.3128	61.2868	239.109888	61.42925	187.011559	75.692319	93.98685674	43.98646489	194.9053	54048.1213888889	2006-11-09 02:54:48	54049.8515509259	2006-11-10 20:26:14	501101010	43.8628	75	79.4274	79.4274	43.8628	79.4194	2	2	2	2	1	0	0	75.8741	75.8741	149.474	1	PROCESSED	57536.1016319444	2016-05-28 02:26:21	54455	2007-12-21 00:00:00	54088.7470486111	2006-12-19 17:55:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011259	We propose to observe the Draco Enhancement, a region of very bright 1/4 keV emission in the northern Galactic halo that is only 15 degrees from the Suzaku observation of the North Ecliptic Pole. A decomposition of the spectrum of the Galactic halo by Kuntz & Snowden showed that, to within the uncertainties of the ROSAT All-Sky Survey, the halo emission was composed of two thermal components; a uniform hot component with kT~0.25 keV, and a very patchy soft component with kT~0.1 keV. The soft component is found in only a few isolated regions of the sky, of which the Draco Enhancement is the brightest. This emission is too soft to be studied with XMM. Suzaku will allow us to determine the temperature of the soft component or place very strict upper limits on its temperature.	GALACTIC DIFFUSE EMISSION	5	C	K. KUNTZ		USA	1	AO1	THE SOFT COMPONENT OF THE GALACTIC HALO	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501101010/	Quick Look
678	COMET_8P_TUTTLE-P1-2	27.9946	7.7582	27.33663	7.511628	28.768937	-3.5069	147.87340904	-52.1573456	248.4994	54470.5826041667	2008-01-05 13:58:57	54470.6488310185	2008-01-05 15:34:19	502062020	2.2193	2	2.2193	2.2193	0	2.2193	1	1	0	1	1	0	0	2.164	2.164	5.718	0	PROCESSED	57540.985162037	2016-06-01 23:38:38	54908	2009-03-18 00:00:00	54542.2129166667	2008-03-17 05:06:36	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062020/	Quick Look
679	COMET_8P_TUTTLE-P1-4	28.0997	7.2516	27.442835	7.005266	28.688048	-4.017818	148.34803657	-52.5857522	248.4989	54470.7159143518	2008-01-05 17:10:55	54470.7821527778	2008-01-05 18:46:18	502062040	1.7233	2	1.7233	1.7233	0	1.7233	1	1	0	1	1	0	0	1.4567	1.4567	5.722	0	PROCESSED	57540.9953125	2016-06-01 23:53:15	54908	2009-03-18 00:00:00	54542.2187847222	2008-03-17 05:15:03	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062040/	Quick Look
680	GC_LARGEPROJECT13	264.4001	-31.8052	263.587715	-31.776061	265.18111	-8.457548	356.65040302	-0.04773216	95.4712	54881.6929282407	2009-02-19 16:37:49	54883.0522453704	2009-02-21 01:15:14	503019010	52.7764	50	52.7764	52.7972	0	52.7844	2	2	0	2	1	0	0	42.4395	42.4395	117.4338	0	PROCESSED	57545.6322106482	2016-06-06 15:10:23	54557	2008-04-01 00:00:00	54902.1118171296	2009-03-12 02:41:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503019010/	Quick Look
681	HESS J1800-240B	270.1124	-24.0578	269.347343	-24.056487	270.09306	-0.616951	5.8867537	-0.376417	87.1402	54562.3157523148	2008-04-06 07:34:41	54563.0141666667	2008-04-07 00:20:24	503026010	31.6728	30	31.6728	31.6728	0	31.6728	1	1	0	1	1	0	0	26.7698	26.7698	60.32	1	PROCESSED	57542.2491319444	2016-06-03 05:58:45	54953	2009-05-02 00:00:00	54580.1793402778	2008-04-24 04:18:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030043	H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region.	GALACTIC DIFFUSE EMISSION	5	A	TAKAAKI TANAKA		JAP	3	AO3	OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503026010/	Quick Look
682	VELA JR P25	132.5224	-46.8921	132.101077	-46.704657	159.613489	-60.474295	266.48184745	-1.82836861	347.0024	54653.1675462963	2008-07-06 04:01:16	54653.4335532407	2008-07-06 10:24:19	503037010	13.16	10	13.16	13.16	0	13.16	1	1	0	1	1	0	0	12.4325	12.4325	22.9759	0	PROCESSED	57542.9817476852	2016-06-03 23:33:43	55048	2009-08-05 00:00:00	54679.3166203704	2008-08-01 07:35:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503037010/	Quick Look
683	CYGNUS LOOP (P27)	313.8328	30.0104	313.308096	29.818528	328.031945	45.024246	74.06049539	-9.7037521	49.6211	54599.5480092593	2008-05-13 13:09:08	54600.0494675926	2008-05-14 01:11:14	503063010	22.7843	20	22.7923	22.7843	0	22.8003	2	2	0	2	1	0	0	20.0688	20.0688	43.3239	0	PROCESSED	57542.5253587963	2016-06-03 12:36:31	54975	2009-05-24 00:00:00	54609.1396990741	2008-05-23 03:21:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503063010/	Quick Look
684	VICINITY_OF_PKS_2155-2	330.1861	-29.9649	329.464287	-30.205624	321.680429	-16.673826	18.22929909	-52.62033555	55.8323	54588.3553356482	2008-05-02 08:31:41	54590.7293865741	2008-05-04 17:30:19	503083010	87.3274	80	87.3274	87.3274	0	87.3274	2	2	0	2	1	0	0	75.8451	75.8451	205.1059	3	PROCESSED	57542.4726736111	2016-06-03 11:20:39	54975	2009-05-24 00:00:00	54608.2608912037	2008-05-22 06:15:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030135	The highly ionized absorption lines of OVII, OVIII, and NeIX at z = 0 have been unambiguously detected toward the bright AGN PKS 2155-304 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII, OVIII and NeIX emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas.	GALACTIC DIFFUSE EMISSION	5	A	TOSHISHIGE HAGIHARA		JAP	3	AO3	STUDY OF WARM-HOT GAS TOWARD PKS 2155-304	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503083010/	Quick Look
685	RIM2	311.426	31.5946	310.913676	31.411344	326.171395	47.287726	74.00572356	-7.09996284	246.8661	55153.9497337963	2009-11-18 22:47:37	55154.4843055556	2009-11-19 11:37:24	504006010	26.3059	24	26.3059	26.3059	0	26.3059	1	1	0	1	1	0	0	22.237	22.237	46.1839	0	PROCESSED	57549.4609490741	2016-06-10 11:03:46	55534	2010-12-04 00:00:00	55166.4447916667	2009-12-01 10:40:30	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504006010/	Quick Look
686	RIM3	311.3232	31.2993	310.809596	31.116423	325.884456	47.049295	73.71675058	-7.21258663	246.4181	55154.4849189815	2009-11-19 11:38:17	55155.1204166667	2009-11-20 02:53:24	504007010	21.5566	19	21.5566	21.5566	0	21.5566	2	2	0	2	1	0	0	17.481	17.481	54.9039	0	PROCESSED	57549.4865277778	2016-06-10 11:40:36	55534	2010-12-04 00:00:00	55166.4304166667	2009-12-01 10:19:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504007010/	Quick Look
687	RIM6	314.3771	31.4503	313.858117	31.256512	329.460239	46.161653	75.4881661	-9.14820234	247.047	55155.7987615741	2009-11-20 19:10:13	55156.1745833333	2009-11-21 04:11:24	504010010	14.3275	11	14.3475	14.3435	0	14.3275	2	2	0	2	1	0	0	10.7152	10.7152	32.468	0	PROCESSED	57549.4929513889	2016-06-10 11:49:51	55534	2010-12-04 00:00:00	55166.4272916667	2009-12-01 10:15:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504010010/	Quick Look
688	NEP #1	270.0492	66.5597	270.050416	66.559437	358.096328	89.986108	96.38280784	29.79186901	217.1802	55150.229212963	2009-11-15 05:30:04	55151.1953587963	2009-11-16 04:41:19	504070010	56.3367	50	56.3367	56.3447	0	56.3447	1	1	0	1	1	0	0	41.4345	41.4345	83.4719	2	PROCESSED	57549.3863657407	2016-06-10 09:16:22	54922	2009-04-01 00:00:00	55162.2062268518	2009-11-27 04:56:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041101	We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe.	GALACTIC DIFFUSE EMISSION	5	A	STEVEN SNOWDEN		USA	4	AO4	OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504070010/	Quick Look
689	SEP #2	89.966	-66.5714	89.96805	-66.571581	300.397678	-89.984546	276.39630454	-29.82495373	163.7813	55170.9454166667	2009-12-05 22:41:24	55172.4863194444	2009-12-07 11:40:18	504071010	57.9991	50	58.0071	57.9991	0	58.0071	2	2	0	2	1	0	0	35.4152	35.4152	133.112	1	PROCESSED	57549.7252546296	2016-06-10 17:24:22	54922	2009-04-01 00:00:00	55187.4854398148	2009-12-22 11:39:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041101	We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe.	GALACTIC DIFFUSE EMISSION	5	A	STEVEN SNOWDEN		USA	4	AO4	OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504071010/	Quick Look
690	SEP #4	89.9798	-66.5683	89.981754	-66.568414	282.855223	-89.989511	276.39272547	-29.81946932	185.1981	55192.0059490741	2009-12-27 00:08:34	55193.3995833333	2009-12-28 09:35:24	504075010	49.9566	50	49.9566	49.9566	0	49.9566	2	2	0	2	1	0	0	45.143	45.143	120.3939	1	PROCESSED	57549.980474537	2016-06-10 23:31:53	54922	2009-04-01 00:00:00	55225.3094907407	2010-01-29 07:25:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041101	We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe.	GALACTIC DIFFUSE EMISSION	5	A	STEVEN SNOWDEN		USA	4	AO4	OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504075010/	Quick Look
691	W28_EASTSHELL	270.3727	-23.2858	269.612111	-23.285763	270.332756	0.154633	6.67541903	-0.20080463	88.0003	55617.4542939815	2011-02-25 10:54:11	55620.1723032407	2011-02-28 04:08:07	505006010	99.9816	100	99.9816	99.9816	0	99.9816	2	2	0	2	1	0	0	83.6772	83.6772	234.8157	3	PROCESSED	57601.1152430556	2016-08-01 02:45:57	55287	2010-04-01 00:00:00	55642.1946643518	2011-03-22 04:40:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050002	We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505006010/	Quick Look
692	CYGNUS LOOP 4	312.482	31.9468	311.969326	31.759715	327.592245	47.259949	74.84594636	-7.58533627	81.0154	55301.6216087963	2010-04-15 14:55:07	55301.8912037037	2010-04-15 21:23:20	505012010	12.4535	12	12.4535	12.4535	0	12.4535	2	2	0	2	1	0	0	12.182	12.182	23.2801	1	PROCESSED	57551.2226736111	2016-06-12 05:20:39	55287	2010-04-01 00:00:00	55362.3160763889	2010-06-15 07:35:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505012010/	Quick Look
693	JUPITER	104.585	23.053	103.829387	23.12132	103.399653	0.287954	192.87049462	11.72496816	267.157	56768.1148958333	2014-04-21 02:45:27	56768.2245138889	2014-04-21 05:23:18	508023140	5.2482	160	5.2642	5.2482	0	5.2708	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57614.9659259259	2016-08-14 23:10:56	57212	2015-07-09 00:00:00	56846.5934143518	2014-07-08 14:14:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023140/	Quick Look
694	CYGNUS LOOP 13	313.3172	30.1574	312.794183	29.967347	327.529928	45.333203	73.89066537	-9.26489611	82.0018	55329.8397337963	2010-05-13 20:09:13	55330.4925694444	2010-05-14 11:49:18	505021010	21.565	21	21.565	21.597	0	21.565	2	2	0	2	1	0	0	18.12	18.12	56.3999	1	PROCESSED	57551.5081597222	2016-06-12 12:11:45	55287	2010-04-01 00:00:00	55393.3656712963	2010-07-16 08:46:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505021010/	Quick Look
695	CYGNUS LOOP 15	313.2124	29.6854	312.687356	29.495723	327.15263	44.932937	73.46064198	-9.49078141	50.2914	55343.3019791667	2010-05-27 07:14:51	55343.6994675926	2010-05-27 16:47:14	505023010	19.2953	19	19.2953	19.2953	0	19.2953	1	1	0	1	1	0	0	16.514	16.514	34.32	1	PROCESSED	57551.5915972222	2016-06-12 14:11:54	55287	2010-04-01 00:00:00	55355.1545833333	2010-06-08 03:42:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505023010/	Quick Look
696	WESTERLUND1_1	251.8398	-46.6023	250.920426	-46.513379	256.432477	-24.011612	339.00946678	-0.92860911	283.3468	55449.7733217593	2010-09-10 18:33:35	55451.2015740741	2010-09-12 04:50:16	505049010	51.932	50	51.932	51.932	0	51.932	2	2	0	2	1	0	0	44.8437	44.8437	123.3861	1	PROCESSED	57553.3910532407	2016-06-14 09:23:07	55829	2011-09-25 00:00:00	55461.3235069444	2010-09-22 07:45:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050078	TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster.	GALACTIC DIFFUSE EMISSION	5	A	HIRONORI MATSUMOTO		JAP	5	AO5	IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505049010/	Quick Look
697	THE KEPLER SNR	262.6712	-21.4826	261.921958	-21.445277	263.170111	1.784866	4.52498243	6.82361728	97.9009	55634.5331712963	2011-03-14 12:47:46	55635.5759606482	2011-03-15 13:49:23	505092060	46.4961	100	46.6401	46.4961	0	46.6401	2	2	0	2	1	0	0	38.6118	38.6118	90.05	1	PROCESSED	57601.1934143518	2016-08-01 04:38:31	55287	2010-04-01 00:00:00	55648.2987731482	2011-03-28 07:10:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092060/	Quick Look
698	CYGNUS LOOP W-B-N	311.1498	30.6623	310.633359	30.480063	325.327706	46.517719	73.11766027	-7.48614398	71.1125	55692.7736574074	2011-05-11 18:34:04	55693.7709606482	2011-05-12 18:30:11	506007010	45.9006	44	45.9006	45.9006	0	45.9006	2	2	0	2	1	0	0	40.8337	40.8337	86.1339	0	PROCESSED	57602.0331597222	2016-08-02 00:47:45	56072	2012-05-25 00:00:00	55705.1432523148	2011-05-24 03:26:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060042	The Cygnus Loop is a prototypical middle-aged SNR. Based on our previous observations, the shell region shows relatively low temperature with low metal abundance. The interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Its abundance non-uniformity indicates the asymmetric explosion. There are two blow-out features: a south-break with one degree diameter and a west-break with half degree diameter. The west-break shows a half-moon shape indicating a rapid expansion in a tenuous plasma. We propose to observe the west-break with SUZAKU for 100 ksec. The plasma in the west-break must be a pure fossil plasma of the SN. We want to study the plasma structure that is almost free from obscuration by the ISM.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	6	AO6	HUNT FOR THE FOSSIL OF THE PROGENITOR STAR IN THE WEST BREAK OF THE CYGNUS LOOP SUPERNOVA REMNANT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506007010/	Quick Look
699	CYGNUS LOOP BLOWOUT4	312.6611	29.185	312.13473	28.997294	326.258052	44.653722	72.76042835	-9.42856877	61.4261	55707.9937268518	2011-05-26 23:50:58	55708.6620486111	2011-05-27 15:53:21	506014010	26.0551	25	26.0551	26.0631	0	26.0711	2	2	0	2	1	0	0	20.2713	20.2713	57.7379	0	PROCESSED	57602.1387037037	2016-08-02 03:19:44	56092	2012-06-14 00:00:00	55725.2494097222	2011-06-13 05:59:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060053	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	6	AO6	MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506014010/	Quick Look
700	S147_NE	85.8826	28.3008	85.092656	28.278902	86.363834	4.912026	180.30181638	-0.72311498	273.9004	55996.1741666667	2012-03-10 04:10:48	55997.2919097222	2012-03-11 07:00:21	506030010	48.0142	45	48.0302	48.0142	0	48.0382	2	2	0	2	1	0	0	42.608	42.608	96.5559	0	PROCESSED	57604.8622685185	2016-08-04 20:41:40	56385	2013-04-03 00:00:00	56016.6658912037	2012-03-30 15:58:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060080	We propose to observe the very old supernova remnant (SNR) S147 with Suzaku/XIS. S147 has a jet like structure suggesting that it was a core collapse supernova. The formation mechanism of the jet remains unclear for the progenitor which has a small mass and creates a neutron star by its explosion. An asymmetric explosion causes a inhomogeneous metallicity abundance. Therefore, we investigate the inhomogeneous by the plasma diagnosis in the X-ray band to obtain the evidence of the jet formation. This will be the limit of theoretical model for the supernova explosion. S147 is also the GeV gamma-ray source. Therefore, we can study the acceleration mechanism of the cosmic rays in the very old SNR if we detect the nonthermal X-ray emission from it.	GALACTIC DIFFUSE EMISSION	5	C	YOSHITAKA HANABATA		JAP	6	AO6	STUDYING THE SUPERNOVA REMNANT S147 WITH JET STRUCTURE AND GEV GAMMA-RAY EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506030010/	Quick Look
701	VELA PWN NE1	129.3684	-44.9817	128.942936	-44.80588	153.830902	-60.001311	263.62243766	-2.36980886	142.6395	55916.6230439815	2011-12-21 14:57:11	55917.0070601852	2011-12-22 00:10:10	506041010	15.408	15	15.424	15.408	0	15.424	1	1	0	1	1	0	0	11.5681	11.5681	33.1759	1	PROCESSED	57604.1925347222	2016-08-04 04:37:15	56305	2013-01-13 00:00:00	55937.7788310185	2012-01-11 18:41:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	C	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506041010/	Quick Look
702	VELA PWN E2	129.5733	-45.3227	129.149771	-45.146105	154.428094	-60.221749	263.98172095	-2.46094632	304.5019	55711.9038773148	2011-05-30 21:41:35	55712.1328935185	2011-05-31 03:11:22	506045010	13.904	15	13.92	13.904	0	13.92	1	1	0	1	1	0	0	8.404	8.404	19.7759	0	PROCESSED	57602.1624074074	2016-08-02 03:53:52	56092	2012-06-14 00:00:00	55725.2563888889	2011-06-13 06:09:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506045010/	Quick Look
703	FERMI_BUBBLE_N1	234.2494	5.0833	233.629011	5.247167	230.509588	23.755664	11.24626366	44.86747445	287.5001	56144.9615277778	2012-08-05 23:04:36	56145.3981365741	2012-08-06 09:33:19	507001010	21.0485	20	21.0485	21.0485	0	21.0485	1	1	0	1	1	0	0	17.5275	17.5275	37.7199	1	PROCESSED	57606.7753703704	2016-08-06 18:36:32	56533	2013-08-29 00:00:00	56167.2004166667	2012-08-28 04:48:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507001010/	Quick Look
704	FERMI_BUBBLE_N8	234.713	2.1937	234.081258	2.355767	231.775859	21.073749	8.32709248	42.83416107	287.4999	56148.4316782407	2012-08-09 10:21:37	56148.9953240741	2012-08-09 23:53:16	507008010	22.115	20	22.119	22.115	0	22.123	3	2	0	2	1	0	0	22.3246	22.3246	48.694	0	PROCESSED	57606.8152546296	2016-08-06 19:33:58	56536	2013-09-01 00:00:00	56169.1379976852	2012-08-30 03:18:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507008010/	Quick Look
705	FERMI_BUBBLE_S5	332.6607	-46.1905	331.884331	-46.436996	316.726495	-32.387556	351.01438321	-53.09632639	44.0062	56036.5915625	2012-04-19 14:11:51	56037.1140972222	2012-04-20 02:44:18	507013010	21.0044	20	21.0124	21.0204	0	21.0044	2	2	0	2	1	0	0	20.8854	20.8854	45.1099	0	PROCESSED	57605.2184259259	2016-08-05 05:14:32	56420	2013-05-08 00:00:00	56049.260787037	2012-05-02 06:15:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507013010/	Quick Look
706	MBM16	49.7705	11.5801	49.086905	11.399033	50.445581	-6.509248	170.60706006	-37.27124926	254.3335	56691.5957175926	2014-02-03 14:17:50	56693.5209953704	2014-02-05 12:30:14	508078020	87.8509	80	87.8509	87.8589	0	87.8589	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57613.7866782407	2016-08-13 18:52:49	56383	2013-04-01 00:00:00	56706.5234375	2014-02-18 12:33:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086002	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	8	AO8	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508078020/	Quick Look
707	GC_SOUTH_4	268.4148	-29.4524	267.616941	-29.442757	268.602472	-6.019039	0.45858363	-1.77042753	273.9837	56206.6347106482	2012-10-06 15:13:59	56207.6987731482	2012-10-07 16:46:14	507031010	52.8743	50	52.8903	52.8903	0	52.8743	1	1	0	1	1	0	0	54.1402	54.1402	91.9199	0	PROCESSED	57607.3059837963	2016-08-07 07:20:37	56595	2013-10-30 00:00:00	56226.5383449074	2012-10-26 12:55:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070042	We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation.	GALACTIC DIFFUSE EMISSION	5	A	SHINYA NAKASHIMA		JAP	7	AO7	OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507031010/	Quick Look
708	G32.8-0.1 NORTH	282.8355	-0.0511	282.194351	-0.111437	283.93132	22.770824	32.87550481	-0.00195799	74.4992	56037.6100347222	2012-04-20 14:38:27	56038.7897685185	2012-04-21 18:57:16	507035010	55.1475	50	55.1475	55.1475	0	55.1475	3	2	0	2	1	0	0	53.4834	53.4834	101.9259	0	PROCESSED	57605.250162037	2016-08-05 06:00:14	56421	2013-05-09 00:00:00	56054.2396990741	2012-05-07 05:45:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070047	A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem.	GALACTIC DIFFUSE EMISSION	5	B	AYA BAMBA		JAP	7	AO7	SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507035010/	Quick Look
709	W44_SOUTH	284.0612	1.21	283.425992	1.143849	285.397736	23.902065	34.55680978	-0.51750637	254.9998	56587.9436921296	2013-10-22 22:38:55	56589.5105671296	2013-10-24 12:15:13	508003010	66.7193	100	66.7333	66.7284	0	66.7193	3	3	0	3	1	0	0	59.54	59.54	135.3439	0	PROCESSED	57613.1119675926	2016-08-13 02:41:14	57193	2015-06-20 00:00:00	56603.6796180556	2013-11-07 16:18:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080012	W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	8	AO8	MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508003010/	Quick Look
710	W28_SOUTH	270.2594	-23.5602	269.497229	-23.559609	270.228192	-0.119534	6.38554367	-0.24638203	269.9307	56938.465162037	2014-10-08 11:09:50	56939.7308101852	2014-10-09 17:32:22	508006020	61.7346	60	61.7346	61.7385	0	61.7465	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6318402778	2016-08-16 15:09:51	57359	2015-12-03 00:00:00	56993.4258333333	2014-12-02 10:13:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080017	A series of discoveries of recombining plasma (RP) in mixed-morphology (MM) SNRs inspires us with a new scenario for SNR evolution. The observed spectra are well described by the picture that the plasma has experienced sudden cooling in the past and currently undergoes gradual recombination to ionization equilibrium. In the MM SNR W28, we found the spatial correlation between the radio brightness and the thermal evolution (recombination) phase. Hence, the radio-fainter region may have less recombined plasma. Such a plasma should emit strong Fe-K line from the He-like ions. The line flux reflects the initial temperature of RP, which brings the key information of the explosion environment of MM SNRs. For this purpose, we propose a 100-ks observation of W28 south, the possible 'youngest' RP.	GALACTIC DIFFUSE EMISSION	5	A	MAKOTO SAWADA		JAP	8	AO8	INITIAL PARAMETERS OF RECOMBINING PLASMA IN SUPERNOVA REMNANTS EXPLORED THROUGH W28	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508006020/	Quick Look
711	NW_BGD	233.685	-9.8963	233.005634	-9.73009	233.775325	9.095249	355.50550051	35.80785483	289.7923	56499.8451041667	2013-07-26 20:16:57	56500.4266319445	2013-07-27 10:14:21	508008010	24.1275	20	24.1275	24.1275	0	24.1275	2	2	0	2	1	0	0	22.0402	22.0402	50.216	1	PROCESSED	57612.0809953704	2016-08-12 01:56:38	56955	2014-10-25 00:00:00	56587.4600578704	2013-10-22 11:02:29	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080020	Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble.	GALACTIC DIFFUSE EMISSION	5	B	MASAYA TAHARA		JAP	8	AO8	SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508008010/	Quick Look
712	CAS A	350.8384	58.8278	350.272774	58.553239	27.387727	54.868389	111.73335389	-2.11549771	73.3126	56828.040162037	2014-06-20 00:57:50	56828.7711111111	2014-06-20 18:30:24	508011020	28.0732	30	28.0812	28.0732	0	29.7402	3	3	0	3	1	0	0	30.9971	30.9971	63.1439	2	PROCESSED	57615.2981712963	2016-08-15 07:09:22	57206	2015-07-03 00:00:00	56839.7807986111	2014-07-01 18:44:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080021	We will propose a follow-up 120 ksec observations of a young supernova remnant Cassiopeia A. The long exposure provides us a high quality of the broad band spectrum from XIS to HXD GSO band. We will try to detect Mn-K line at 6.1 keV for the first time. The element Mn as well as Cr gives constraint on the explosion mechanism of the ejecta. We also test a predicted flux variation of a non-thermal emission in the PIN band for the first time. The variation gives critical information to solve the physical parameters in the reverse shock of the ejecta.	GALACTIC DIFFUSE EMISSION	5	B	YOSHITOMO MAEDA		JAP	8	AO8	MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508011020/	Quick Look
713	HESS J1641-463	250.6069	-46.2544	249.692976	-46.159834	255.458921	-23.78613	338.71856162	-0.05766971	282.1914	56898.1501736111	2014-08-29 03:36:15	56898.2719907407	2014-08-29 06:31:40	509010010	0	40	0	0	0	0	0	0	0	0	0	0	0	0	0	0	0	PROCESSED	57616.5288773148	2016-08-16 12:41:35	56748	2014-04-01 00:00:00	56979.4106944445	2014-11-18 09:51:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090045	The origin of cosmic rays has been one of the biggest problems in modern astrophysics. TeV gamma-ray observations provide indirect evidences of cosmic ray acceleration, although the sources detected so far have softer spectra than what would be expected by particle accelerators to explain the observed distribution of cosmic rays at the knee. HESS J1641-463 is the hardest TeV gamma-ray source ever found. With Suzaku's large effective area, and low and stable background, we will perform the first deep X-ray observation of this source to seek for its X-ray counterpart, and to identify its nature. It will provide a direct look into the physics of the highest energy particle accelerators in our Galaxy, responsible for the cosmic ray spectrum up to the spectral knee at PeV energies.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	9	AO9	IDENTIFYING THE X-RAY COUNTERPART OF THE HARDEST SOURCE HUMAN EVER DETECTED	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509010010/	Quick Look
714	G166.0+4.3_SE	81.6669	42.6537	80.773056	42.61122	83.513405	19.400906	166.36639381	4.14814693	85.0186	56921.2402777778	2014-09-21 05:46:00	56922.0209606482	2014-09-22 00:30:11	509024010	31.2731	60	31.2731	34.2171	0	34.2731	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.5684722222	2016-08-16 13:38:36	57626	2016-08-26 00:00:00	56945.4935532407	2014-10-15 11:50:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090092	Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation.	GALACTIC DIFFUSE EMISSION	5	A	AKIHIRO TAKATA		JAP	9	AO9	G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509024010/	Quick Look
715	MONOGEM RING WEST	118.3557	8.2507	117.679197	8.381467	118.769502	-12.402687	212.50229712	17.5030797	287.8334	53865.545462963	2006-05-10 13:05:28	53867.1127199074	2006-05-12 02:42:19	501084010	54.2685	50	54.2685	54.2685	54.2685	54.2685	2	2	2	2	1	0	0	43.2312	43.2312	135.3899	2	PROCESSED	57534.3136689815	2016-05-26 07:31:41	54401	2007-10-28 00:00:00	53914.2479282407	2006-06-28 05:57:01	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011243	We propose to acquire the first high-quality, CCD resolution spectrum of the Monogem Ring SNR. The Monogem Ring is a large (D~25 degrees), old (t~10^5 yr) SNR with a soft X-ray spectrum. A 50 ks observation with Suzaku will detect and measure the OVII Triplet and OVIII Lyman-alpha line fluxes. We will use the ratio of these two line complexes to constrain the temperature and ionization timescale of the plasma in this region of the Monogem Ring. Determing the plasma conditions in such evolved SNRs is important for understanding how these remnants merge with and affect the interstellar medium.	GALACTIC DIFFUSE EMISSION	5	B	PAUL PLUCINSKY		USA	1	AO1	THE MONOGEM RING: MEASURING THE O LINE EMISSION WITH SUZAKU	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501084010/	Quick Look
716	RCW86_NORTH	220.4956	-62.2074	219.51679	-61.994077	240.607034	-43.72111	315.43082177	-2.04872285	96.1584	54860.901099537	2009-01-29 21:37:35	54862.1175231482	2009-01-31 02:49:14	503002010	55.376	50	55.384	55.384	0	55.376	2	2	0	2	1	0	0	50.2731	50.2731	105.0818	2	PROCESSED	57545.4267939815	2016-06-06 10:14:35	55329	2010-05-13 00:00:00	54880.5551041667	2009-02-18 13:19:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030011	Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		JAP	3	AO3	RCW86 MAPPING OBSERVATION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503002010/	Quick Look
717	KES 79	283.1953	0.6959	282.557686	0.633849	284.399792	23.479242	33.70438491	0.01846016	73.5801	55674.9437152778	2011-04-23 22:38:57	55676.4716782407	2011-04-25 11:19:13	506059010	50.897	50	50.897	50.897	0	50.897	2	2	0	2	1	0	0	40.8978	40.8978	131.96	2	PROCESSED	57601.597025463	2016-08-01 14:19:43	55652	2011-04-01 00:00:00	55697.1427083333	2011-05-16 03:25:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506059010/	Quick Look
718	3C400.2 NE	294.7841	17.3445	294.222174	17.229031	300.592872	38.189932	53.75798011	-2.26924911	81.5891	56770.0289351852	2014-04-23 00:41:40	56770.4640162037	2014-04-23 11:08:11	509071010	20.231	20	20.239	20.239	0	20.231	1	1	0	1	1	0	0	18.505	18.505	37.5838	0	PROCESSED	57614.9798148148	2016-08-14 23:30:56	57152	2015-05-10 00:00:00	56789.6056712963	2014-05-12 14:32:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092010	Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances.	GALACTIC DIFFUSE EMISSION	5	A	JACCO VINK		EUR	9	AO9	THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509071010/	Quick Look
719	W63	304.8117	45.7821	304.405742	45.623994	328.881818	62.294552	82.4091518	5.43831098	57.9996	57171.5134837963	2015-05-29 12:19:25	57172.616712963	2015-05-30 14:48:04	510025010	42.7003	150	44.302	44.606	0	42.7003	2	2	0	2	1	0	0	13.7747	13.7747	92.7739	0	PROCESSED	57618.8028703704	2016-08-18 19:16:08	57636	2016-09-05 00:00:00	57260.7216898148	2015-08-26 17:19:14	3.0.22.44	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101315	We propose to conduct a deep Suzaku observation of the X-ray bright central portion of the Galactic supernova remnant (SNR) W63 (G82.2+5.3). This SNR belongs to a class of objects known as mixed-morphology SNRs (MMSNRs) that feature a shell-like radio morphology with a center-filled thermal X-ray morphology: the origin of these contrasting morphologies for these SNRs remains unknown. Our proposed Suzaku observation of this SNR will investigate the putative overabundances of such elements as magnesium, silicon and sulfur (as reported in a previous analysis of an ASCA observation of W63) as well as search for evidence of over-ionization conditions in the X-ray emitting plasma, as has been reported for other MMSNRs.	GALACTIC DIFFUSE EMISSION	5	C	THOMAS PANNUTI		USA	10	AO10	A SUZAKU OBSERVATION OF THE GALACTIC SUPERNOVA REMNANT W63 (G82.2+5.3)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/510025010/	Quick Look
720	CYGNUS_LOOP_P15	312.9857	30.6621	312.465734	30.473222	327.433989	45.909388	74.106397	-8.72540127	61.9987	53880.177974537	2006-05-25 04:16:17	53880.6716898148	2006-05-25 16:07:14	501032010	20.7289	21	20.7289	20.7289	20.7289	20.7289	2	2	2	2	1	0	0	17.476	17.476	42.6349	0	PROCESSED	57534.4101041667	2016-05-26 09:50:33	54394	2007-10-21 00:00:00	53926.2440046296	2006-07-10 05:51:22	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501032010/	Quick Look
721	GC19	265.8593	-28.4466	265.068242	-28.424576	266.336192	-5.058113	0.1669402	0.66404713	262.6738	54384.9647569444	2007-10-11 23:09:15	54385.4112731482	2007-10-12 09:52:14	502007010	22.0174	20	22.0174	22.0414	0	22.0254	2	2	0	2	1	0	0	19.5248	19.5248	38.572	0	PROCESSED	57540.2498842593	2016-06-01 05:59:50	54771	2008-11-01 00:00:00	54402.4381365741	2007-10-29 10:30:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502007010/	Quick Look
722	VELA JR P16	132.6844	-46.1051	132.256587	-45.917087	158.947915	-59.751955	265.94403391	-1.24290223	347.0001	54291.4605671296	2007-07-10 11:03:13	54291.7363773148	2007-07-10 17:40:23	502038010	16.442	10	16.45	16.45	0	16.442	1	1	0	1	1	0	0	16.277	16.277	23.8239	1	PROCESSED	57539.143900463	2016-05-31 03:27:13	54696	2008-08-18 00:00:00	54328.4979398148	2007-08-16 11:57:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502038010/	Quick Look
723	COMET_8P_TUTTLE-P1-7	28.2572	6.4878	27.602012	6.241824	28.565429	-4.78789	149.08057764	-53.2281425	248.4991	54470.9158333333	2008-01-05 21:58:48	54470.9820717593	2008-01-05 23:34:11	502062070	3.219	2	3.219	3.219	0	3.219	1	1	0	1	1	0	0	3.459	3.459	5.664	0	PROCESSED	57541.0036805556	2016-06-02 00:05:18	54908	2009-03-18 00:00:00	54542.2385532407	2008-03-17 05:43:31	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062070/	Quick Look
724	GC_LARGEPROJECT12	264.5561	-31.5945	263.745071	-31.566119	265.306919	-8.241878	356.89942182	-0.04701536	96.416	54881.313900463	2009-02-19 07:32:01	54881.6919444445	2009-02-19 16:36:24	503018030	11.914	10	11.922	11.922	0	11.914	2	2	0	2	1	0	0	10.0909	10.0909	32.6579	1	PROCESSED	57545.5776041667	2016-06-06 13:51:45	54557	2008-04-01 00:00:00	54895.5872106482	2009-03-05 14:05:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503018030/	Quick Look
725	HESSJ1614-B	243.5783	-51.8962	242.621623	-51.770198	251.47747	-30.138638	331.46625372	-0.63583262	283.7142	54730.5632291667	2008-09-21 13:31:03	54731.2779166667	2008-09-22 06:40:12	503074010	52.6342	50	52.6422	52.6342	0	52.6342	2	2	0	2	1	0	0	42.953	42.953	61.7359	0	PROCESSED	57543.9760763889	2016-06-04 23:25:33	55148	2009-11-13 00:00:00	54780.4609490741	2008-11-10 11:03:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030088	The TeV image of HESSJ1614-518 is double peaked, and we observed one of them during the AO-1 with the Suzaku XIS. We discovered extended X-ray emission which coincides with the TeV emission. Then we propose to observe the other peak. We also found a bright object between the double peaks. HESSJ1614 may be a pulsar wind nebula, and the object may be a pulsar driving the nebula. However, the object was just at the edge of the XIS field of view, we could not study it in detail. Then, we propose another position to observe the object. Furthermore, we discovered soft diffuse emission around HESSJ1614. We propose the other position to study the spatial extension of the diffuse emission.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	3	AO3	MAPPING OBSERVATION OF HESSJ1614-518	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503074010/	Quick Look
726	VELA JR P19	133.9797	-46.1476	133.547729	-45.954999	160.484775	-59.304415	266.55257885	-0.58147519	346.9993	54650.629849537	2008-07-03 15:06:59	54651.2362731482	2008-07-04 05:40:14	503031010	19.8174	10	19.8174	19.8174	0	19.8174	2	2	0	2	1	0	0	17.1564	17.1564	52.3839	1	PROCESSED	57542.9517824074	2016-06-03 22:50:34	55036	2009-07-24 00:00:00	54665.3240393518	2008-07-18 07:46:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503031010/	Quick Look
727	KEPLER_BG_GN	261.9141	-20.2308	261.17196	-20.189852	262.396131	2.997058	5.199252	8.09662946	270.3619	55105.4689699074	2009-10-01 11:15:19	55107.4279976852	2009-10-03 10:16:19	504103010	68.6043	60	68.6043	68.6043	0	68.6123	2	2	0	2	1	0	0	55.8014	55.8014	169.2279	1	PROCESSED	57548.7547800926	2016-06-09 18:06:53	54922	2009-04-01 00:00:00	55125.6331828704	2009-10-21 15:11:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	4	AO4	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504103010/	Quick Look
728	G276.2-7.7	135.4479	-58.0976	135.120843	-57.899721	179.6274	-67.871169	276.2324482	-7.68832918	319.4197	56102.2534722222	2012-06-24 06:05:00	56102.610625	2012-06-24 14:39:18	507066010	10.2994	10	10.2994	10.2994	0	10.2994	1	1	0	1	1	0	0	11.6275	11.6275	30.8559	0	PROCESSED	57605.7340972222	2016-08-05 17:37:06	56582	2013-10-17 00:00:00	56219.6536458333	2012-10-19 15:41:15	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072014	We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed.	GALACTIC DIFFUSE EMISSION	5	A	TOBIAS PRINZ		EUR	7	AO7	IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507066010/	Quick Look
729	VELA PWN S2	128.0787	-47.1859	127.674645	-47.014943	154.605433	-62.350481	264.85904608	-4.40317226	122.1879	56989.4162847222	2014-11-28 09:59:27	56989.8404976852	2014-11-28 20:10:19	509018010	17.4774	15	17.4774	17.4774	0	17.4774	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.4063773148	2016-08-17 09:45:11	57368	2015-12-12 00:00:00	57002.436087963	2014-12-11 10:27:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090046	We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	9	AO9	X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509018010/	Quick Look
730	G189 NORTH	94.8937	22.8595	94.136063	22.881413	94.510579	-0.50482	189.05453502	3.64004382	92.0693	56941.8561458333	2014-10-11 20:32:51	56944.6669328704	2014-10-14 16:00:23	509035010	100.65	100	100.65	102.898	0	102.922	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.652337963	2016-08-16 15:39:22	57362	2015-12-06 00:00:00	56996.4204282407	2014-12-05 10:05:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091314	We propose observations of G189.6+3.3, a large candidate supernova remnant (SNR) that overlaps with the much better studied remnant IC 443. Little is known about G189; ROSAT images show a shell-like structure about 1.5$^{circ}$ in diameter, but it has never been observed with modern X-ray telescopes. Its association, or lack thereof, with IC 443 is unknown. It may not be a supernova remnant at all; a superbubble origin for the X-ray emission also provides an intriguing possibility. Spatially-resolved spectroscopy with Suzaku will allow the detailed measurement of the plasma properties, illuminating the nature of this object. Determining the nature of G189 will help to probe the evolution of the ISM driven by the deaths of massive stars.	GALACTIC DIFFUSE EMISSION	5	B	BRIAN WILLIAMS		USA	9	AO9	OBSERVATIONS OF G189.6+3.3: AN SNR COMPANION TO IC 443?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509035010/	Quick Look
731	SNR 0103-72.6	16.2944	-72.389	15.898915	-72.656584	313.931508	-65.2662	301.47055063	-44.70024477	13.8765	53848.0156018518	2006-04-23 00:22:28	53849.3773032407	2006-04-24 09:03:19	501077010	49.2715	50	49.2795	49.2875	49.2875	49.2715	2	2	2	2	1	0	0	37.1905	37.1905	117.6299	3	PROCESSED	57533.5571296296	2016-05-25 13:22:16	54401	2007-10-28 00:00:00	53907.4220023148	2006-06-21 10:07:41	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011241	We propose Suzaku observations of O-rich supernova remnants (SNRs) 0103-72.6 and 0049-73.6 in the Small Magellanic Cloud (SMC). These SMC SNRs are oldest members (18000 and 14000 yr old) of O-rich SNRs and share X-ray spectral characteristics with a young (1000 yr old) O-rich SNR 0102-7219 which is also in the SMC. While sharing similar spectral features with 0102-7219, the morphologies of 0103-72.6 and 0049-73.6 indicate more evolved phases of the SNR in a similar interstellar environment as 0102-7219. Cross-comparison studies with the high spectral resolution Suzaku/XIS observations among 0103-72.6/0049-73.6 (this proposal) and 0102-7219 (scheduled/observed for the instrument calibrations) will provide a unique opportunity for the study of a long-term evolution of an O-rich SNR.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	1	AO1	BACK TO THE FUTURE: LONG-TERM EVOLUTION OF OXYGET-RICH SUPERNOVA REMNANTS IN THE SMALL MAGELLANIC CLOUD	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501077010/	Quick Look
732	HESS J1745-303 2	266.4705	-30.0867	265.668866	-30.067612	266.916061	-6.683329	359.0474588	-0.64781783	70.5003	54531.5601388889	2008-03-06 13:26:36	54533.6669444444	2008-03-08 16:00:24	502017010	72.5443	67	72.5523	72.5523	0	72.5443	2	2	0	2	1	0	0	63.9723	63.9723	182.0149	2	PROCESSED	57541.8457291667	2016-06-02 20:17:51	54919	2009-03-29 00:00:00	54550.4057986111	2008-03-25 09:44:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020023	A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku.	GALACTIC DIFFUSE EMISSION	5	B	RYO YAMAZAKI		JAP	2	AO2	SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502017010/	Quick Look
733	ARC_BACKGROUND	39.2055	-35.7283	38.691278	-35.944876	20.761341	-47.725244	240.48717091	-66.02341726	233.8071	54830.2554861111	2008-12-30 06:07:54	54835.3468055556	2009-01-04 08:19:24	503104010	201.8775	140	201.9575	201.8775	0	201.9815	2	2	0	2	1	0	0	5.5028	5.5028	14.506	0	PROCESSED	57545.0672685185	2016-06-06 01:36:52	55328	2010-05-12 00:00:00	54851.4354166667	2009-01-20 10:27:00	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031235	Aside from the lengthy bright arcs in the northern sky, few X-ray bright, high latitude regions are understood. Yet, studying this gas is important for understanding the Galactic halo. Here, we propose to study a medium-sized (~7 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make Suzaku observations of the arc and nearby background. With them and an existing Suzaku observation, we will be able to determine the thermal properties of the arc plasma and if the arc is the bright limb of a hot bubble.	GALACTIC DIFFUSE EMISSION	5	B	ROBIN SHELTON		USA	3	AO3	A CLOSER LOOT AT HOT HALO GAS: A SUZAKU STUDY OF AN X-RAY BRIGHT ARC	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503104010/	Quick Look
734	ASO0382	265.491	-20.8915	264.744419	-20.867803	265.774532	2.483348	6.43327069	4.9108593	101.5727	55276.7369328704	2010-03-21 17:41:11	55277.3869675926	2010-03-22 09:17:14	504040010	21.2223	20	21.2223	21.2223	0	21.2223	2	2	0	2	1	0	0	3.974	3.974	56.1089	2	PROCESSED	57550.9335069444	2016-06-11 22:24:15	55665	2011-04-14 00:00:00	55299.411875	2010-04-13 09:53:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 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 DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504040010/	Quick Look
735	PUP A : BEK	125.942	-42.9405	125.511174	-42.777913	147.596211	-59.401563	260.51799115	-3.16426215	276.3687	53842.2933449074	2006-04-17 07:02:25	53842.5807407407	2006-04-17 13:56:16	501086010	16.0913	15	16.0913	16.0993	16.0913	16.0913	1	1	1	1	1	0	0	9.6985	9.6985	24.797	0	PROCESSED	57533.4850115741	2016-05-25 11:38:25	54401	2007-10-28 00:00:00	53906.8467708333	2006-06-20 20:19:21	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501086010/	Quick Look
736	COMET_8P_TUTTLE-P1_BGD-2	28.5654	5.0072	27.913501	4.76193	28.330895	-6.281929	150.57128999	-54.45813442	248.5002	54471.5006018518	2008-01-06 12:00:52	54471.6876273148	2008-01-06 16:30:11	502061020	5.6821	4	5.6901	5.6821	0	5.6967	1	1	0	1	1	0	0	5.598	5.598	16.1519	0	PROCESSED	57541.2728819444	2016-06-02 06:32:57	54908	2009-03-18 00:00:00	54542.2619097222	2008-03-17 06:17:09	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502061020/	Quick Look
737	COMET_8P_TUTTLE-P1_BGD-1	28.5142	5.254	27.861749	5.008612	28.370132	-6.032929	150.31676982	-54.25438929	248.4996	54471.3338888889	2008-01-06 08:00:48	54471.5001273148	2008-01-06 12:00:11	502061010	8.39	6	8.39	8.39	0	8.39	1	1	0	1	1	0	0	7.4419	7.4419	14.3439	0	PROCESSED	57541.2728935185	2016-06-02 06:32:58	54908	2009-03-18 00:00:00	54542.2616319444	2008-03-17 06:16:45	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502061010/	Quick Look
738	COMET_8P_TUTTLE-P1-13	28.5683	5.0085	27.916397	4.763237	28.334076	-6.281727	150.57488577	-54.45575395	248.5007	54471.3158333333	2008-01-06 07:34:48	54471.3334606482	2008-01-06 08:00:11	502062130	0	0	0	0	0	0	0	0	0	0	0	0	0	0	0	1.5039	0	PROCESSED	57541.2672337963	2016-06-02 06:24:49	54910	2009-03-20 00:00:00	54544.4202893518	2008-03-19 10:05:13	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062130/	Quick Look
739	G296.1-0.5S	177.6962	-62.7172	177.080034	-62.439005	216.307928	-55.355417	296.04515802	-0.65925146	111.5869	54482.7727662037	2008-01-17 18:32:47	54484.6668402778	2008-01-19 16:00:15	502069010	69.213	67	69.213	69.213	0	69.213	2	2	0	2	1	0	0	61.0096	61.0096	163.6237	2	PROCESSED	57541.3665740741	2016-06-02 08:47:52	54929	2009-04-08 00:00:00	54563.4417824074	2008-04-07 10:36:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021218	Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles.	GALACTIC DIFFUSE EMISSION	5	C	KAZIMIERZ BORKOWSKI		USA	2	AO2	G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502069010/	Quick Look
740	EXTENDED CHIMNEY	265.9856	-29.2095	265.189699	-29.188076	266.46906	-5.817544	359.57541621	0.16970004	69.9995	54896.1105555556	2009-03-06 02:39:12	54899.1218171296	2009-03-09 02:55:25	503072010	140.5733	133	140.5733	140.5733	0	140.5733	2	2	0	2	1	0	0	135.4784	135.4784	260.128	1	PROCESSED	57545.7802546296	2016-06-06 18:43:34	55330	2010-05-14 00:00:00	54916.5067361111	2009-03-26 12:09:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030086	We have discovered a chimney structure in the Sgr C region with Suzaku. The Suzaku spectrum of the chimney shows typical parameters of a super nova remnant. However, the chimney has a linear shape, which is inconsistent with a SNR. Thus, we are considering that the chimney is a blowout from super bubble in the Sgr C region. Another possible scenario is that the chimney would be a part of a shell structure formed by explosions (starburst activities, Sgr A*, magnetic reconnection) in the region of Sgr A and Sgr C. Thus, in this proposal, we would like to investigate the structure extending from the chimney.	GALACTIC DIFFUSE EMISSION	5	B	TAKESHI TSURU		JAP	3	AO3	THE CHIMNEY OF SGR C : A PART OF A SUPER BUBBLE = A SUPER SHELL ?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503072010/	Quick Look
741	G12.8-0.0	273.3975	-17.831	272.667266	-17.845732	273.239831	5.571499	12.81826803	-0.01988984	90.5577	54894.8233680556	2009-03-04 19:45:39	54896.1050810185	2009-03-06 02:31:19	503087010	56.2026	50	56.2026	56.2026	0	56.2059	2	2	0	2	1	0	0	51.5312	51.5312	110.7278	1	PROCESSED	57545.7287962963	2016-06-06 17:29:28	55329	2010-05-13 00:00:00	54908.5701388889	2009-03-18 13:41:00	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031203	By studying pulsar wind nebulae, the synchrotron nebulae powered by a neutron star's loss of rotational energy, it is possible to determine the energetics of both the progenitor supernova and central neutron star. This requires estimates of the expansion velocity and mass swept-up the pulsar wind nebulae, best obtained by analyzing the spectrum of the thermal X-rays emitting by this material. In the proposal, we request a 50ks observation of four of the most energetic pulsar wind nebulae in the Milky Way to both detect such thermal X-ray emission and use the measured spectral properties to infer the ejecta mass and kinetic energy of their progenitor supernova and the initial spin period of the central neutron star -- all currently unmeasurable using the currently available information.	GALACTIC DIFFUSE EMISSION	5	C	JOSEPH GELFAND		USA	3	AO3	STUDYING THE PROGENITOR SUPERNOVA AND CENTRAL NEUTRON STAR OF PULSAR WIND NEBULAE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503087010/	Quick Look
742	BLOWOUT4	312.7282	31.6832	312.213719	31.495234	327.721378	46.935084	74.77065214	-7.91349372	242.7253	55160.4733564815	2009-11-25 11:21:38	55161.0044444445	2009-11-26 00:06:24	504014010	17.7696	15	17.8257	17.7696	0	17.8256	3	2	0	2	1	0	0	14.2657	14.2657	45.876	0	PROCESSED	57549.5615509259	2016-06-10 13:28:38	55545	2010-12-15 00:00:00	55176.2692939815	2009-12-11 06:27:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504014010/	Quick Look
743	GALACTICDISC3-2	16.1096	72.7817	15.228315	72.513728	58.016186	57.534015	123.90816526	9.93459858	241.5401	55216.0250115741	2010-01-20 00:36:01	55217.5772685185	2010-01-21 13:51:16	504039010	73.5282	70	73.5282	73.5282	0	73.5282	2	2	0	2	1	0	0	54.648	54.648	134.1058	1	PROCESSED	57550.3049884259	2016-06-11 07:19:11	55602	2011-02-10 00:00:00	55236.1178240741	2010-02-09 02:49:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040097	To elucidate the vertical structure of the yet-not-understood excess soft X-ray emission from the galactic disk, we propose to observe two offset directions from the plane along l = 123 degree. We expect the spectra contains the 0.75 keV emission component which we discovered in the energy spectra of two midplane observations. The proposed observations will strongly constrain the nature of the sources which are responsible for the excess emission, in particular the vertical distribution in the Galaxy.	GALACTIC DIFFUSE EMISSION	5	C	SHUNSUKE KIMURA		JAP	4	AO4	STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504039010/	Quick Look
744	G348.5+0.1	258.6301	-38.5295	257.772536	-38.472556	260.783274	-15.450832	348.44223752	0.09652262	91.401	55247.6321180556	2010-02-20 15:10:15	55248.7592476852	2010-02-21 18:13:19	504097010	53.8106	50	53.8106	53.8106	0	53.8106	2	2	0	2	1	0	0	46.3929	46.3929	97.3598	1	PROCESSED	57550.6723842593	2016-06-11 16:08:14	54922	2009-04-01 00:00:00	55257.0343287037	2010-03-02 00:49:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504097010/	Quick Look
745	CYGNUS LOOP 16	312.8966	29.5255	312.371396	29.336949	326.707962	44.890523	73.15999246	-9.37678246	49.3574	55343.7003125	2010-05-27 16:48:27	55344.4932407407	2010-05-28 11:50:16	505024010	34.8338	34	34.8338	34.8338	0	34.8338	2	2	0	2	1	0	0	32.4182	32.4182	68.5079	1	PROCESSED	57551.6200231482	2016-06-12 14:52:50	55287	2010-04-01 00:00:00	55355.2000115741	2010-06-08 04:48:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505024010/	Quick Look
746	0534-69.9	83.5094	-69.9134	83.62618	-69.94462	302.596953	-85.878508	280.47493809	-31.97334872	273.4822	55286.3873726852	2010-03-31 09:17:49	55289.2981597222	2010-04-03 07:09:21	505064010	109.2367	100	109.2687	109.2367	0	109.2767	2	2	0	2	1	0	0	79.8262	79.8262	251.4437	2	PROCESSED	57551.1453819445	2016-06-12 03:29:21	55287	2010-04-01 00:00:00	55302.4291898148	2010-04-16 10:18:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051102	Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors.	GALACTIC DIFFUSE EMISSION	5	A	KAZIMIERZ BORKOWSKI		USA	5	AO5	TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505064010/	Quick Look
747	GALACTIC_BULGE18	269.3126	-34.5716	268.480017	-34.566233	269.41346	-11.131891	356.40349802	-4.99577293	70.9023	55633.4308101852	2011-03-13 10:20:22	55634.5273263889	2011-03-14 12:39:21	505087010	51.4284	50	51.4684	51.4284	0	51.4755	1	1	0	1	1	0	0	44.2072	44.2072	94.7279	1	PROCESSED	57601.1565046296	2016-08-01 03:45:22	55287	2010-04-01 00:00:00	55649.0417824074	2011-03-29 01:00:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505087010/	Quick Look
748	HB21 SOUTH	311.2245	50.5821	310.838387	50.399364	342.625257	64.000491	88.82715261	4.80607932	6.557	55767.8922337963	2011-07-25 21:24:49	55768.4953819444	2011-07-26 11:53:21	506005020	23.4607	20	23.4687	23.4767	0	23.4607	2	2	0	2	1	0	0	26.2649	26.2649	52.1039	1	PROCESSED	57602.6622685185	2016-08-02 15:53:40	56159	2012-08-20 00:00:00	55792.1611458333	2011-08-19 03:52:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060011	Over-ionization in SNRs is one of the biggest mystery Suzaku discovered. It affects a lot the study on chemical and thermal evolution of universe, but the origin is still unknown. HB21 is an old SNR with molecular cloud interaction and GeV gamma-rays, which remind us typical over-ionization SNRs. On the other hand, the interacting molecular cloud is much smaller or thinner than those interacting with over-ionization SNRs, and as a result, HB21 can be the key target to study the origin of over-ionization. Suzaku deep observation of HB21 south (interacting point) will determine the condition of plasma and judge whether it is in over-ionization or not, which will show us the origin of over-ionizing plasma.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	6	AO6	ORIGIN OF OVER-IONIZATION OF SNR PLASMAS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506005020/	Quick Look
749	JUPITER	28.6779	10.4549	28.01316	10.209883	30.347447	-1.217435	147.25964186	-49.40473582	249.1856	55929.8714467593	2012-01-03 20:54:53	55930.8243865741	2012-01-04 19:47:07	506006010	33.5331	160	33.5331	33.5331	0	33.5331	2	2	0	2	1	0	0	32.1369	32.1369	82.3239	1	PROCESSED	57604.310625	2016-08-04 07:27:18	56316	2013-01-24 00:00:00	55946.1978472222	2012-01-20 04:44:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060017	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter.	GALACTIC DIFFUSE EMISSION	5	B	KUMI ISHIKAWA		JAP	6	AO6	STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006010/	Quick Look
750	G352.7-0.1	261.9227	-35.1119	261.088463	-35.070764	263.245639	-11.859611	352.75195989	-0.12120729	94.0335	55988.8605671296	2012-03-02 20:39:13	55993.5536111111	2012-03-07 13:17:12	506052010	201.5474	200	201.5474	201.5474	0	201.5474	2	2	0	2	1	0	0	171.544	171.544	405.4396	4	PROCESSED	57604.9422569445	2016-08-04 22:36:51	56375	2013-03-24 00:00:00	56008.397337963	2012-03-22 09:32:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061315	Supernova remnants showing strong Fe K emission are relatively rare, and primarily of Type Ia. We propose a long observation of one of the least well-studied Fe-rich Galactic SNRs, G352.7-0.1, with the goal of characterizing the Fe emission, confirming its likely identification as the remnant of a Type Ia supernova, and constraining the properties of ejected material and the dynamics of the explosion. Its thermal X-ray spectrum is strikingly similar to Tycho's SNR, but unexpectedly X-rays are uniformly distributed throughout the remnant. Our proposed observation will produce high-quality spectra, adequate for detailed studies with some spatial information, that will greatly aid in understanding of this very interesting young remnant.	GALACTIC DIFFUSE EMISSION	5	C	KAZIMIERZ BORKOWSKI		USA	6	AO6	STRONG IRON EMISSION IN THE SUPERNOVA REMNANT G352.7-0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506052010/	Quick Look
751	VELA JR WEST1	131.7706	-46.5645	131.349361	-46.379775	158.374389	-60.478179	265.90247722	-2.02224689	126.9994	56630.5848611111	2013-12-04 14:02:12	56631.1640162037	2013-12-05 03:56:11	508036010	28.5509	30	28.5589	28.5589	0	28.5509	2	2	0	2	1	0	0	27.35	27.35	50.0179	0	PROCESSED	57613.5034375	2016-08-13 12:04:57	57061	2015-02-08 00:00:00	56695.6005092593	2014-02-07 14:24:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080082	We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution.	GALACTIC DIFFUSE EMISSION	5	C	HIDETOSHI SANO		JAP	8	AO8	FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508036010/	Quick Look
752	CYGNUS_LOOP_P19	311.8094	30.0818	311.288879	29.89716	325.768852	45.764417	73.00862935	-8.2918477	237.4997	54087.3411805556	2006-12-18 08:11:18	54087.8245833333	2006-12-18 19:47:24	501036010	18.595	17	18.595	18.595	0	18.595	2	2	0	2	1	0	0	18.355	18.355	41.7559	0	PROCESSED	57536.3627199074	2016-05-28 08:42:19	54744	2008-10-05 00:00:00	54096.1443171296	2006-12-27 03:27:49	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501036010/	Quick Look
753	GALACTIC RIDGE	281.0036	-4.078	280.343207	-4.129572	281.600756	18.920487	28.45707071	-0.21069081	265.5303	54023.0938888889	2006-10-15 02:15:12	54025.8141087963	2006-10-17 19:32:19	500009020	98.8583	100	98.8743	98.8663	98.8583	98.8743	2	2	2	2	1	0	0	81.9519	81.9519	235.0139	1	PROCESSED	57535.9070023148	2016-05-27 21:46:05	54697	2008-08-19 00:00:00	54055.6082407407	2006-11-16 14:35:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001042	We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field.	GALACTIC DIFFUSE EMISSION	5	A	KEN EBISAWA		JAP	0	SWG	ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500009020/	Quick Look
754	MBM12	43.9954	19.5008	43.287121	19.299344	47.246432	2.625648	159.17119109	-34.46234987	73.4994	55776.7501388889	2011-08-03 18:00:12	55780.4398263889	2011-08-07 10:33:21	506026010	150.3202	150	150.3202	150.3202	0	150.3202	2	2	0	2	1	0	0	143.5349	143.5349	280.7618	5	PROCESSED	57602.8321180556	2016-08-02 19:58:15	56169	2012-08-30 00:00:00	55802.465625	2011-08-29 11:10:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060068	We propose an observation toward dense molecular cloud region MBM12 that is in front of the Local Hot Bubble. Solar wind charge exchange induced emission, reacted with neutrals in the heliosphere (H-SWCX), is considered to have significant influence to the soft diffuse X-ray background under 1 keV. However, there is no significant evidence of the H-SWCX. From this observation, we try to reveal the existence of H-SWCX induced emission by comparing the OVII line emission (0.57 keV) with Suzaku archive data. We also aim to constrain the time variability of H-SWCX emission, depending on the 12 year solar activity.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI YOSHITAKE		JAP	6	AO6	OBSERVATION TOWARD MOLECULAR CLOUD MBM12 : VERIFYING SOLAR WIND CHARGE EXCHANGE EMISSION IN THE HELIOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506026010/	Quick Look
755	GRXE_E_9	268.0849	-26.1545	267.307554	-26.143306	268.269555	-2.725006	3.15134991	0.15632851	103.0998	56385.8984490741	2013-04-03 21:33:46	56388.2085648148	2013-04-06 05:00:20	507074010	98.6516	100	98.6596	98.6596	0	98.6516	2	2	0	2	1	0	0	83.0269	83.0269	199.5757	2	PROCESSED	57611.012650463	2016-08-11 00:18:13	56018	2012-04-01 00:00:00	56401.6405092593	2013-04-19 15:22:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507074010/	Quick Look
756	W44_WEST	283.939	1.3216	283.304324	1.256024	285.27764	24.025907	34.60037354	-0.35787423	254.9999	56589.5109953704	2013-10-24 12:15:50	56590.9655324074	2013-10-25 23:10:22	508002010	61.1078	60	61.1398	61.1078	0	61.1398	2	2	0	2	1	0	0	58.4458	58.4458	125.6678	1	PROCESSED	57613.10125	2016-08-13 02:25:48	56970	2014-11-09 00:00:00	56603.7391087963	2013-11-07 17:44:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080012	W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	8	AO8	MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508002010/	Quick Look
757	GRXE_E_7	268.3325	-26.1696	267.555037	-26.159608	268.492207	-2.737339	3.2513581	-0.04270444	86.7249	56716.5321296296	2014-02-28 12:46:16	56718.7084953704	2014-03-02 17:00:14	508076010	102.6848	100	102.6978	102.6868	0	102.6848	2	2	0	2	1	0	0	96.4539	96.4539	188.0198	3	PROCESSED	57613.9520486111	2016-08-13 22:50:57	56383	2013-04-01 00:00:00	56727.7217013889	2014-03-11 17:19:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086001	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	8	AO8	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508076010/	Quick Look
758	DIFFUSE1C	201.9274	6.8104	201.299196	7.069212	197.642152	14.849246	327.54723828	67.93166205	123.897	57015.2219560185	2014-12-24 05:19:37	57015.3450115741	2014-12-24 08:16:49	509060010	5.5117	20	5.5277	5.5197	0	5.5117	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.5590393518	2016-08-17 13:25:01	57417	2016-01-30 00:00:00	57049.4528587963	2015-01-27 10:52:07	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091324	In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them.	GALACTIC DIFFUSE EMISSION	5	C	JOEL BREGMAN		USA	9	AO9	UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509060010/	Quick Look
759	73P/SW3	317.5094	24.3437	316.953773	24.139336	329.181406	38.538464	71.75290875	-15.84652301	72.7094	53868.2758333333	2006-05-13 06:37:12	53868.3418865741	2006-05-13 08:12:19	500013030	3.225	20	3.225	3.225	3.225	3.225	1	1	1	1	1	0	0	2.915	2.915	5.7039	0	PROCESSED	57534.2995023148	2016-05-26 07:11:17	54256	2007-06-05 00:00:00	54042.2712731482	2006-11-03 06:30:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013030/	Quick Look
760	COMET_8P_TUTTLE-P1-1	27.7163	7.989	27.057965	7.741803	28.591929	-3.193745	147.31647839	-52.04673223	248.4436	54470.5233333333	2008-01-05 12:33:36	54470.5821759259	2008-01-05 13:58:20	502062010	0.6803	2	0.6803	0.6803	0	0.6803	1	1	0	1	1	0	0	0.632	0.632	5.08	0	PROCESSED	57540.9802199074	2016-06-01 23:31:31	54908	2009-03-18 00:00:00	54542.4502083333	2008-03-17 10:48:18	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062010/	Quick Look
761	RIM1	311.6421	31.883	311.130799	31.698954	326.587321	47.481782	74.34868893	-7.06658523	247.7276	55152.9451273148	2009-11-17 22:40:59	55153.9488888889	2009-11-18 22:46:24	504005010	40.7473	38	40.7473	40.7473	0	40.7473	2	2	0	2	1	0	0	34.5112	34.5112	86.7159	0	PROCESSED	57549.4623726852	2016-06-10 11:05:49	55534	2010-12-04 00:00:00	55166.4923148148	2009-12-01 11:48:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504005010/	Quick Look
762	SEP #1	89.966	-66.5774	89.968235	-66.57758	292.016086	-89.97915	276.40322057	-29.82494721	141.7136	55149.1175925926	2009-11-14 02:49:20	55150.2141087963	2009-11-15 05:08:19	504069010	51.8621	50	51.8701	51.8621	0	51.8701	2	2	0	2	1	0	0	48.3534	48.3534	94.7259	2	PROCESSED	57549.3577546296	2016-06-10 08:35:10	54922	2009-04-01 00:00:00	55160.1496296296	2009-11-25 03:35:28	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041101	We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe.	GALACTIC DIFFUSE EMISSION	5	A	STEVEN SNOWDEN		USA	4	AO4	OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504069010/	Quick Look
763	W28_CENTER	270.074	-23.3664	269.312952	-23.364911	270.05835	0.07446	6.46943001	-0.00256773	84.9544	55289.3078935185	2010-04-03 07:23:22	55290.9918287037	2010-04-04 23:48:14	505005010	73.0036	70	73.0437	73.0036	0	73.0436	3	2	0	2	1	0	0	57.2981	57.2981	145.4519	2	PROCESSED	57551.1131944444	2016-06-12 02:43:00	55287	2010-04-01 00:00:00	55322.3694675926	2010-05-06 08:52:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050002	We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505005010/	Quick Look
764	FERMI_BUBBLE_N7	234.5505	3.1681	233.922592	3.3308	231.347519	21.977572	9.28415113	43.5333275	287.4999	56147.9630787037	2012-08-08 23:06:50	56148.4306944444	2012-08-09 10:20:12	507007010	22.7991	20	22.8071	22.7991	0	22.8151	2	2	0	2	1	0	0	21.0084	21.0084	40.3999	0	PROCESSED	57606.8138541667	2016-08-06 19:31:57	56536	2013-09-01 00:00:00	56169.1051388889	2012-08-30 02:31:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507007010/	Quick Look
765	W49B	287.7842	9.1154	287.185843	9.031744	290.654437	31.289753	43.28107632	-0.18330097	82.0063	57125.7127893518	2015-04-13 17:06:25	57128.6891087963	2015-04-16 16:32:19	509001020	103.0426	400	103.0426	113.1875	0	113.1795	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.0199537037	2016-08-18 00:28:44	56748	2014-04-01 00:00:00	57142.3645138889	2015-04-30 08:44:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090007	W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	9	AO9	DEEP OBSERVATIONS OF W49B	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001020/	Quick Look
766	HOT BLOB 3	127.507	51.0389	126.590865	51.206602	116.529664	30.99487	167.88407696	36.01101877	263.6154	57139.1338657407	2015-04-27 03:12:46	57140.9141319444	2015-04-28 21:56:21	509009010	81.1183	80	81.1183	81.5423	0	81.5503	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57644.5780902778	2016-09-13 13:52:27	57591	2016-07-22 00:00:00	57224.4589351852	2015-07-21 11:00:52	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090044	Hot blobs including plasma of temperature kT = 0.6 - 1.0 keV in the Milky-Way Halo were found in 1/10 of the sky by systematical analysis of the soft X-ray diffuse background in Suzaku/XIS observations. They can play a role in matter and energy transportation among the Galactic plane, the Milky-Way Halo and intergalactic space. In order to reveal origin and physical condition of them, we focus on the part of a hot blob in (ell, b) = (161.505, 40.696) and propose to observe neighboring this area to constrain its size.	GALACTIC DIFFUSE EMISSION	5	C	NORIO SEKIYA		JAP	9	AO9	ORIGIN AND PHYSICAL CONDITION OF HOT BLOBS IN THE MILKY-WAY HALO	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509009010/	Quick Look

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