DARTS Astro

total 16

No.
target_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
proposal_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
hxd_burst_num
processing_status
processing_end_time_mjd
processing_end_time
public_date_mjd
public_date
distribute_start_date_mjd
distribute_start_date
processing_version
processing_quantity
processing_software
proposal_id
proposal_abstract
proposal_category
proposal_category_code
proposal_priority
pi_name
co_pi_name
proposal_affiliated_country
proposal_cycle_count
observation_type
proposal_title
main_detector
xis_injection_flag
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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