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 16

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	N132D	81.2911	-69.6367	81.393061	-69.678644	312.497631	-85.535647	280.29591185	-32.77442189	319.8518	57144.6915972222	2015-05-02 16:35:54	57145.5405092593	2015-05-03 12:58:20	110007010	31.4878	25	31.4878	31.4878	0	31.4878	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.064837963	2016-08-18 01:33:22	57113	2015-04-01 00:00:00	57164.52875	2015-05-22 12:41:24	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	105001	This is the proposal for the XIS calibration observations in the AO10 cycle.	CALIBRATION	1	A	MASAHIRO TSUJIMOTO		JAP	10	AO10	XIS CALIBRATION OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/110007010/	Quick Look
2	M82 N2	148.2738	70.273	147.216273	70.508377	118.122269	52.466944	140.95732372	40.02876632	282.8972	57162.9827546296	2015-05-20 23:35:10	57164.434224537	2015-05-22 10:25:17	810043010	59.8084	60	59.8084	61.9021	0	61.9021	2	2	0	2	0	0	0	0	0	34.13	0	PROCESSED	57618.7218287037	2016-08-18 17:19:26	57548	2016-06-09 00:00:00	57177.3762847222	2015-06-04 09:01:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101442	We propose to carry out Suzaku observations of the starburst galaxy M82. We will search for X-ray emission from winds and shock heated clouds out to its possible outer boundary of ~45 kpc. We will also constrain the density and temperature profiles of the gas/wind emission out to large radii. These data can place important constraints on theoretical models of starburst galaxies and their environments. We will test models such as the Chevalier & Clegg adiabatic wind model, shocked clouds in a wind, etc. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	10	AO10	SEARCH FOR THE OUTER BOUNDARY OF THE STARBURST GALAXY: M82	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/810043010/	Quick Look
3	EP DRA	286.7359	69.1573	286.793684	69.076999	30.014466	83.210835	100.08892772	23.87463538	44.5637	57164.4409953704	2015-05-22 10:35:02	57166.2856365741	2015-05-24 06:51:19	410006010	80.2346	80	80.2346	80.2426	0	80.2426	2	2	0	2	1	0	0	67.9585	67.9585	155.5819	1	PROCESSED	57618.7517939815	2016-08-18 18:02:35	57558	2016-06-19 00:00:00	57176.3159027778	2015-06-03 07:34:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	100018	It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar mass (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar mass and approach 3.3 solar mass. We will get observational relations between WD mass and radius for proposed targets with Suzaku. With WD masses dynamically measured, we can estimate the WD radii without any theoretical mass-radius relation. We will be able to, for the first time, observationally investigate the influence of magnetic field on EOS in WDs and the WD mass-radius relation by the estimating WD radii and masses.	GALACTIC POINT SOURCES	4	A	TAKAYUKI HAYASHI		JAP	10	AO10	CONSTRAINT ON MASS-RADIUS RELATION OF HIGHLY MAGNETIZED WHITE DWARFS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410006010/	Quick Look
4	CYGNUS X-1	299.5777	35.2112	299.107757	35.074782	313.651801	54.261993	71.33781217	3.08063246	52.2303	57169.4748148148	2015-05-27 11:23:44	57170.7827893518	2015-05-28 18:47:13	410018010	11.0177	50	11.0177	12.2057	0	11.7469	4	3	0	3	1	0	0	26.1315	26.1315	110.7598	0	PROCESSED	57618.8568171296	2016-08-18 20:33:49	57626	2016-08-26 00:00:00	57183.6630902778	2015-06-10 15:54:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101725	We propose to observe Cygnus X-1 with NuSTAR (for 30 ks) and Suzaku (for 50 ks) in any spectral state in order to measure the reflection component and constrain the properties of the inner accretion disk, including the location of the inner radius, the geometry of the hard X-ray source, and the inclination. Observations made in the first two years of the NuSTAR mission have raised the interesting possibility that the inner disk inclination may differ from the orbital inclination, and this could occur if the black hole spin is misaligned. The proposed NuSTAR/Suzaku observation would be at the orbital phase where absorption due to stellar wind material is at a minimum, providing a clean measurement of the iron line profile and a significant improvement over the existing observations.	GALACTIC POINT SOURCES	4	A	JOHN TOMSICK		USA	10	AO10	THE INNER ACCRETION DISK AROUND THE RAPIDLY ROTATING BLACK HOLE IN CYGNUS X-1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410018010/	Quick Look
5	MRK 509	311.0374	-10.7203	310.356339	-10.901854	310.541946	7.132317	35.97290357	-29.85106035	73.7532	57143.3705671296	2015-05-01 08:53:37	57144.6814930556	2015-05-02 16:21:21	410017010	54.2728	50	54.2757	54.2757	0	54.2728	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.0659722222	2016-08-18 01:35:00	57593	2016-07-24 00:00:00	57225.3881944445	2015-07-22 09:19:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101708	We propose combined Suzaku 50~ks and NuSTAR 200~ks observations of the bright Seyfert 1 galaxy Mrk~509 for the purpose of making a detailed study of the spectrum of radiation reflected from the accretion disk. Our chief aim is to constrain both the spin of the black hole and the properties of the corona that illuminates the disk. The combination of NuSTAR's high-sensitivity in the hard X-ray band, the soft-band coverage of Suzaku, and our state-of-the-art relativistic reflection models will allow us to break degeneracies between different scenarios currently proposed to explain the broadband spectrum of this exceptionally bright and much-studied source.	GALACTIC POINT SOURCES	4	A	JAVIER GARCIA		USA	10	AO10	OBSERVING THE STRONG-FIELD REGION OF THE AGN IN MRK~509	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410017010/	Quick Look
6	NGC 2788A	135.6754	-68.2181	135.519975	-68.019146	206.346244	-72.761691	284.17134554	-14.14937336	282.2863	57157.0478819444	2015-05-15 01:08:57	57158.2230324074	2015-05-16 05:21:10	710007010	42.2339	40	42.2339	42.2339	0	42.2339	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.6656828704	2016-08-18 15:58:35	57591	2016-07-22 00:00:00	57224.447650463	2015-07-21 10:44:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	100009	Swift/BAT extragalactic survey above E >15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe four Compton thick AGN candidates in the 70 month BAT catalog with Suzaku. Since their spectra below 10 keV are likely reflection dominated, joint analysis of Suzaku/XIS and Swift/BAT can constrain the absorption and intrinsic luminosity without being much affected by time variability. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep survey.	EXTRAGALACTIC COMPACT SOURCES	7	B	YOSHIHIRO UEDA		JAP	10	AO10	DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710007010/	Quick Look
7	ARK 564	340.6583	29.7351	340.07073	29.472916	355.35057	34.71587	92.13955378	-25.32593551	75.7895	57167.0898842593	2015-05-25 02:09:26	57168.4029282407	2015-05-26 09:40:13	710018010	52.5104	50	52.5104	53.9344	0	53.9344	2	2	0	2	1	0	0	27.9802	27.9802	100.9477	2	PROCESSED	57618.7636921296	2016-08-18 18:19:43	57548	2016-06-09 00:00:00	57178.248587963	2015-06-05 05:57:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	102721	A NuSTAR legacy is emerging through long observations of bare Seyfert galaxies that reveal an unprecedented look at relativistic reflection off an ionized accretion disc. We propose now to look at the Seyfert galaxy Ark 564 for 200 ks with NuSTAR and 50 ks with Suzaku in order to understand the reflection in this bright source. Ark 564 has been well-studied in the soft band, revealing a steep spectrum, strong soft excess, broad iron K emission line and dramatic variability on the order of hours. It is very akin to two other well-known bare Seyferts, 1H0707-405 and IRAS 13224-3809, except it is an order of magnitude brighter. With this 200 ks observation, we will probe the geometry of the corona, through a complete spectral and timing analysis.	EXTRAGALACTIC COMPACT SOURCES	7	B	ERIN KARA		EUR	10	AO10	UNDERSTANDING REFLECTION IN THE BARE SEYFERT I ARK 564	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710018010/	Quick Look
8	OJ 287	133.705	20.1043	132.989927	20.295379	130.505973	2.596868	206.81753743	35.82068078	285.8744	57148.4467708333	2015-05-06 10:43:21	57151.4189351852	2015-05-09 10:03:16	710011020	110.2819	323	110.2819	112.3099	0	112.3099	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.1271643518	2016-08-18 03:03:07	57113	2015-04-01 00:00:00	57164.5272337963	2015-05-22 12:39:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101431	Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously.	EXTRAGALACTIC COMPACT SOURCES	7	A	RICK EDELSON		USA	10	AO10	SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011020/	Quick Look
9	OJ 287	133.7049	20.1044	132.989827	20.295479	130.505855	2.596938	206.81738245	35.82062575	285.8744	57151.4189467593	2015-05-09 10:03:17	57154.3266666667	2015-05-12 07:50:24	710011030	107.7143	323	107.7143	107.7143	0	107.7143	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.6879166667	2016-08-18 16:30:36	57113	2015-04-01 00:00:00	57164.5596527778	2015-05-22 13:25:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101431	Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously.	EXTRAGALACTIC COMPACT SOURCES	7	A	RICK EDELSON		USA	10	AO10	SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011030/	Quick Look
10	ANTLIA NW4	156.477	-34.4731	155.913183	-34.218342	174.203454	-40.552676	271.69853818	19.42589093	299.2985	57168.4177546296	2015-05-26 10:01:34	57169.4605902778	2015-05-27 11:03:15	810066010	6.3596	40	6.3596	6.8635	0	6.8635	3	2	0	2	1	0	0	6.7341	6.7341	78.0621	0	PROCESSED	57618.7963657407	2016-08-18 19:06:46	57626	2016-08-26 00:00:00	57178.2408101852	2015-06-05 05:46:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101522	We have measured hot gas properties of the nearest non-cool core cluster, Antlia, in the eastern direction out to R200. Our initial results suggest that its density profile is more consistent with some massive clusters, but significantly steeper than its cool core counterpart with a similar temperature (mass), Virgo. We propose to extend our program to observe two other directions to test azimuthal variation, which is likely to be significant. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KA-WAH WONG		USA	10	AO10	MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/810066010/	Quick Look
11	MKN 6	103.0685	74.413	101.450971	74.472117	95.572656	51.225087	140.3435691	26.1094153	254.4482	57133.5883333333	2015-04-21 14:07:12	57134.7015046296	2015-04-22 16:50:10	710001010	50.6541	50	50.6541	51.3396	0	51.3396	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.0317476852	2016-08-18 00:45:43	57548	2016-06-09 00:00:00	57154.4415162037	2015-05-12 10:35:47	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101730	We request two quasi-simultaneous NuSTAR + Suzaku-XIS pointings of the radio-loud Sy 1.5 Mkn 6 to understand the complexity of its accreting circumnuclear gas structures. A series of high-quality, broadband X-ray spectra, including coverage above 10 keV, are needed to properly quantify the variable and complex line of sight absorbers. These new observations, in conjunction with radio and previous X-ray observations, will be a unique opportunity to understand accretion modes in the innermost regions of a radio-loud AGN that has recently undergone a merger.	EXTRAGALACTIC COMPACT SOURCES	7	A	ALEX MARKOWITZ		USA	10	AO10	COMPLEX CIRCUMNUCLEAR ABSORPTION IN RADIO-LOUD AGN: VARIABLE ABSORPTION IN MKN 6	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710001010/	Quick Look
12	NGC 3516	166.6817	72.5579	165.82888	72.82825	123.376111	57.97325	133.24892211	42.40929053	306.0068	57154.3345023148	2015-05-12 08:01:41	57157.0348611111	2015-05-15 00:50:12	710009010	117.7012	120	117.7012	123.0032	0	124.7632	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.6915277778	2016-08-18 16:35:48	57593	2016-07-24 00:00:00	57224.4439467593	2015-07-21 10:39:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	100040	In the AO-8 cycle, we have proposed several X-ray and optical simultaneous observations of a type I Seyfert galaxy NGC 3516, and obtained a good correlation between those wavelengths in its faint phase. The result suggests that a hard primary X-ray continua found in NGC 3516 by Noda et al. (2013) is generated in a corona formed closely to an accretion disk, which is possibly a radiatively inefficient accretion flow. As a next step, we examine whether or not an X-ray variation is also correlated with that in optical, when NGC 3516 is in the bright phase, and the other primary X-ray continuum, also reported by Noda et al. (2013), is dominant. For it, we propose an X-ray and optical simultaneous observation of NGC 3516 with an exposure of 120 ksec, which is triggered by a Swift monitoring.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	10	AO10-TOO	X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF NGC 3516 IN ITS BRIGHT PHASE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710009010/	Quick Look
13	OJ 287	133.7046	20.1043	132.989527	20.295378	130.505611	2.596765	206.8173824	35.82032681	285.8742	57145.5508449074	2015-05-03 13:13:13	57148.4467592593	2015-05-06 10:43:20	710011010	111.6388	323	111.6388	111.6388	0	111.6388	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.1122800926	2016-08-18 02:41:41	57113	2015-04-01 00:00:00	57164.5257523148	2015-05-22 12:37:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101431	Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously.	EXTRAGALACTIC COMPACT SOURCES	7	A	RICK EDELSON		USA	10	AO10	SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011010/	Quick Look
14	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
15	M81	148.8829	69.0533	147.858629	69.290285	119.502258	51.56628	142.10623941	40.90540672	287.1391	57160.4721180556	2015-05-18 11:19:51	57162.9807523148	2015-05-20 23:32:17	710017010	97.7022	100	97.7022	99.738	0	99.7444	3	2	0	2	0	0	0	0	0	0.3	0	PROCESSED	57618.7210532407	2016-08-18 17:18:19	57543	2016-06-04 00:00:00	57177.3710300926	2015-06-04 08:54:17	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	102700	We propose to observe the Low-Luminosity Active Galactic Nucleus of M81 for 200 ksec with NuSTAR and for 100 ksec with Suzaku. In low accretion rate AGN, where does the optically thick part of the accretion disk stop? Does it go in to within a few gravitational radii of the black hole, as in higher accretion rate Seyfert galaxies, or does it stop hundreds of gravitational radii from the black hole? Using NuSTAR and Suzaku spectra we will measure the strengths of the Compton reflection hump, Fe K alpha, Fe XXV and Fe XXVI lines. This will determine whether the Fe K alpha line is produced by reflection off the optically thick outer disk, or is produced in the optically thin inner flow. We will measure the reflection fraction and constrain the source geometry and disk transition radius.	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREW YOUNG		EUR	10	AO10	M81: ACCRETION GEOMETRY AT LOW EDDINGTON RATES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710017010/	Quick Look
16	SXDB2	305.4808	37.2375	305.012336	37.076849	322.528101	54.400691	75.63404607	0.19419319	72.9993	57170.7872453704	2015-05-28 18:53:38	57171.5090972222	2015-05-29 12:13:06	410014010	29.3922	30	29.3959	29.3947	0	29.3922	3	3	0	3	0	0	0	0	0	0	0	PROCESSED	57618.772650463	2016-08-18 18:32:37	57558	2016-06-19 00:00:00	57190.4609259259	2015-06-17 11:03:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	100037	The soft X-ray sky below 1 keV is spatially smooth after subtracting the local extended emission structures although the interstellar X-ray absorption column density is high enough to block the extragalactic X-ray photons below 1 keV totally in the Galactic disk. Suzaku reveals the existence of "excess" emissions in the Galactic disk and our observations will allow us to study a spatial distribution of the emissions and constrain the origin.	GALACTIC POINT SOURCES	4	C	IKUYUKI MITSUISHI		JAP	10	AO10	EXPLORING THE ORIGIN OF SOFT X-RAY DIFFUSE BACKGROUND IN THE GALACTIC DISK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410014010/	Quick Look

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