DARTS Astro

total 503

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 GX 349+2 256.427 -36.366 255.587548 -36.298664 258.786235 -13.451096 349.14511841 2.78820606 85.6584 53808.5453240741 2006-03-14 13:05:16 53809.2216782407 2006-03-15 05:19:13 400003010 25.2308 50 25.2308 25.2332 25.2308 25.2308 1 1 1 1 1 0 0 20.0507 20.0507 58.434 2 PROCESSED 57533.2006365741 2016-05-25 04:48:55 54247 2007-05-27 00:00:00 54041.9132060185 2006-11-02 21:55:01 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 001026 We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure. GALACTIC POINT SOURCES 4 A HIROMITSU TAKAHASHI JAP 0 SWG SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES) HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400003010/ Quick Look
2 SS CYG 325.6789 43.5736 325.187819 43.344381 350.451149 52.649921 90.55119171 -7.12024619 276.5788 53676.0503703704 2005-11-02 01:12:32 53676.9856944444 2005-11-02 23:39:24 400006010 39.4512 40 39.4512 39.4512 39.4512 39.4512 2 2 2 2 1 0 0 32.0472 32.0472 80.81 1 PROCESSED 57527.7175925926 2016-05-19 17:13:20 54247 2007-05-27 00:00:00 54036.9898148148 2006-10-28 23:45:20 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 001043 Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst. GALACTIC POINT SOURCES 4 A MANABU ISHIDA JAP 0 SWG SS CYG OBSERVATION IN QUIESCENCE N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400006010/ Quick Look
3 X1630-472 248.4706 -47.343 247.550146 -47.238721 254.054156 -25.085181 336.93140696 0.30212129 69.0657 53781.9791087963 2006-02-15 23:29:55 53782.5474305556 2006-02-16 13:08:18 400010020 21.429 200 21.429 21.485 21.429 21.429 2 2 2 2 1 0 0 17.0223 17.0223 49.1019 0 PROCESSED 57533.0117592593 2016-05-25 00:16:56 54247 2007-05-27 00:00:00 54041.4892013889 2006-11-02 11:44:27 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 001058 We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. GALACTIC POINT SOURCES 4 A JEAN COTTAM JAP 0 SWG-TOO FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010020/ Quick Look
4 JUPITER 226.5694 -16.1887 225.870685 -15.99606 228.664382 1.239883 343.96536778 35.7224308 118.4901 53790.7643402778 2006-02-24 18:20:39 53791.7940277778 2006-02-25 19:03:24 401001010 37.7594 36 37.7674 37.7594 37.7674 37.7674 2 2 2 2 1 0 0 32.8361 32.8361 88.9361 1 PROCESSED 57533.0781597222 2016-05-25 01:52:33 54401 2007-10-28 00:00:00 53905.533900463 2006-06-19 12:48:49 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011003 We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. GALACTIC POINT SOURCES 4 C RONALD ELSNER USA 1 AO1 JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001010/ Quick Look
5 SS 433 287.9527 4.99 287.334904 4.905608 290.182673 27.181461 39.69879316 -2.23786427 78.6446 53833.4611458333 2006-04-08 11:04:03 53834.4579166667 2006-04-09 10:59:24 401004010 40.1976 40 40.2216 40.1976 40.2296 40.2136 2 2 2 2 1 0 0 30.4749 30.4749 86.11 2 PROCESSED 57533.4357638889 2016-05-25 10:27:30 54400 2007-10-27 00:00:00 53906.5501736111 2006-06-20 13:12:15 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 010031 SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber. GALACTIC POINT SOURCES 4 A NOBUYUKI KAWAI JAP 1 AO1 SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401004010/ Quick Look
6 1E1207.4-5209 182.4916 -52.442 181.83735 -52.163724 209.144209 -45.784625 296.53791481 9.91413144 148.6893 54146.2087384259 2007-02-15 05:00:35 54147.6390509259 2007-02-16 15:20:14 401030020 49.8266 50 50.0734 49.8266 0 50.0894 1 2 0 1 1 0 0 44.4468 44.4468 123.576 2 PROCESSED 57537.4372337963 2016-05-29 10:29:37 54750 2008-10-11 00:00:00 54153.9886458333 2007-02-22 23:43:39 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 010152 1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object. GALACTIC POINT SOURCES 4 B ATSUMASA YOSHIDA JAP 1 AO1 A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401030020/ Quick Look
7 HR 9024 357.4125 36.4308 356.782155 36.152799 14.165064 34.009987 109.27773456 -24.79729068 49.8624 53939.0616782407 2006-07-23 01:28:49 53940.6016087963 2006-07-24 14:26:19 401032010 58.7757 60 58.7997 58.7757 58.7837 58.7917 2 2 2 2 1 0 0 56.0116 56.0116 133.0398 1 PROCESSED 57535.042025463 2016-05-27 01:00:31 54401 2007-10-28 00:00:00 53950.2624074074 2006-08-03 06:17:52 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011022 Suzaku-XIS is the best available instrument to study the Fe fluorescence emission from late-type evolved stars. Fe fluorescence is produced by illumination of the photosphere by ionizing coronal X-rays and its intensity depends on the height of the X-ray source. We propose to observe Fe fluorescence in the single G-type giant HR 9024 and in the active RS CVn system II Peg to obtain a direct geometrical constraint on the scale height of their coronal structures. These two stars have the brightest Fe fluorescence features of all the late-type stars observed by the Chandra-HETGS and their different stellar parameters (stellar radius, gravity, multiplicity,..) and evolutionary stage will allow us to probe the typical coronal scale for significantly different conditions. GALACTIC POINT SOURCES 4 B PAOLA TESTA USA 1 AO1 GEOMETRY DIAGNOSTICS FROM FE FLUORESCENT EMISSION IN LATE-TYPE EVOLVED STARS XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401032010/ Quick Look
8 BETA LYR 282.5098 33.3716 282.047998 33.312385 288.857806 55.996493 63.19266924 14.79477853 53.4974 53867.1260185185 2006-05-12 03:01:28 53867.6252199074 2006-05-12 15:00:19 401036020 21.4962 20 21.4962 21.4962 21.4962 21.4962 1 1 1 1 1 0 0 19.1642 19.1642 43.1199 2 PROCESSED 57534.2764814815 2016-05-26 06:38:08 54401 2007-10-28 00:00:00 53914.2784143518 2006-06-28 06:40:55 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011031 The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. GALACTIC POINT SOURCES 4 A RICHARD IGNACE USA 1 AO1 AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036020/ Quick Look
9 4U 1705-44 257.2295 -44.1004 256.326357 -44.0367 260.194477 -21.092135 343.32321952 -2.34240238 264.0794 53976.2429166667 2006-08-29 05:49:48 53976.7731712963 2006-08-29 18:33:22 401046010 18.3155 20 18.3155 18.3155 18.3155 18.3155 2 2 2 2 1 0 0 15.3715 15.3715 45.8099 0 PROCESSED 57535.3889236111 2016-05-27 09:20:03 54526 2008-03-01 00:00:00 54021.306087963 2006-10-13 07:20:46 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011112 We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. GALACTIC POINT SOURCES 4 A ANDREW YOUNG USA 1 AO1 REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046010/ Quick Look
10 4U 1636-536 250.2262 -53.7541 249.22979 -53.657603 256.460667 -31.236861 332.91086545 -4.81751491 91.2457 54140.3877546296 2007-02-09 09:18:22 54140.99125 2007-02-09 23:47:24 401050010 24.232 19 24.232 24.232 0 24.232 2 1 0 2 1 0 0 21.6895 21.6895 52.136 0 PROCESSED 57537.3410069445 2016-05-29 08:11:03 54525 2008-02-29 00:00:00 54151.5052893518 2007-02-20 12:07:37 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011117 Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. GALACTIC POINT SOURCES 4 A JEROEN HOMAN USA 1 AO1 THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050010/ Quick Look
11 IGRJ16195-4945 244.8541 -49.816 243.916706 -49.695602 251.909406 -27.940354 333.49117084 0.29973526 284.0301 53998.8508333333 2006-09-20 20:25:12 53999.7231481482 2006-09-21 17:21:20 401056010 39.1486 40 39.1486 39.1486 39.1486 39.1486 2 2 2 2 1 0 0 42.2652 42.2652 75.3579 1 PROCESSED 57535.652662037 2016-05-27 15:39:50 54526 2008-03-01 00:00:00 54020.9227199074 2006-10-12 22:08:43 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011132 INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. GALACTIC POINT SOURCES 4 A RANDALL SMITH USA 1 AO1 HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401056010/ Quick Look
12 CYGNUS X-1 299.6124 35.133 299.141904 34.996436 313.652571 54.178807 71.28577556 3.01567368 256.2202 54038.1501273148 2006-10-30 03:36:11 54038.8225 2006-10-30 19:44:24 401059010 27.7068 30 27.7068 27.7378 27.7068 27.7068 2 1 2 2 1 0 0 27.6892 27.6892 58.0839 0 PROCESSED 57535.9949768518 2016-05-27 23:52:46 54526 2008-03-01 00:00:00 54063.4924884259 2006-11-24 11:49:11 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011141 We request three, 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. GALACTIC POINT SOURCES 4 B MICHAEL NOWAK USA 1 AO1 ENHANCING THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401059010/ Quick Look
13 V1223 SGR 283.7445 -31.105 282.940068 -31.169256 281.851865 -8.228404 5.0082738 -14.31987205 79.9528 54203.4803240741 2007-04-13 11:31:40 54204.9418055556 2007-04-14 22:36:12 402002010 60.706 60 60.706 60.706 0 60.706 2 2 0 2 1 0 0 46.2861 46.2861 126.2719 2 PROCESSED 57538.1822800926 2016-05-30 04:22:29 54744 2008-10-05 00:00:00 54210.6596875 2007-04-20 15:49:57 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 020008 The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS. GALACTIC POINT SOURCES 4 A MANABU ISHIDA JAP 2 AO2 MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402002010/ Quick Look
14 PSR B1259-63 195.6556 -63.8839 194.86632 -63.61523 227.712317 -50.941906 304.16255435 -1.03887935 293.4832 54304.2811226852 2007-07-23 06:44:49 54304.6877777778 2007-07-23 16:30:24 402014050 19.7023 20 19.7023 19.7023 0 19.7023 1 1 0 1 1 0 0 17.7549 17.7549 35.1279 0 PROCESSED 57539.3024768518 2016-05-31 07:15:34 54707 2008-08-29 00:00:00 54339.2175347222 2007-08-27 05:13:15 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 020059 We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. GALACTIC POINT SOURCES 4 A YASUNOBU UCHIYAMA JAP 2 AO2 THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014050/ Quick Look
15 LS 5039 276.5633 -14.9109 275.848755 -14.941003 276.400444 8.383997 16.82651822 -1.31880921 270.412 54352.6780555556 2007-09-09 16:16:24 54358.4725 2007-09-15 11:20:24 402015010 203.2399 200 203.2399 203.2399 0 203.2399 2 2 0 2 1 0 0 181.095 181.095 442.0879 4 PROCESSED 57540.0947685185 2016-06-01 02:16:28 54745 2008-10-06 00:00:00 54384.7259027778 2007-10-11 17:25:18 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 020062 The periodicity of TeV gamma-rays from the Galactic microquasar LS 5039 has recently been detected by the HESS Cherenkov telescope. We propose to conduct a simultaneous X-ray/VHE gamma-ray observations for a total of 200 ks of the microquasar with Suzaku XIS and HXD in conjuction with the HESS telescope. A full orbital period of 3.9 days is planned to be covered with Suzaku and HESS. The goal of this program is to study a possible correlation of X-TeV fluxes and spectral changes as a function of orbital phase, thereby shedding a new light on the origin of high-energy radiation from the microquasar system. GALACTIC POINT SOURCES 4 A TADAYUKI TAKAHASHI JAP 2 AO2 SIMULTANEOUS SUZAKU AND HESS OBSERVATIONS OF THE TEV GAMMA-RAY MICROQUASAR LS 5039 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402015010/ Quick Look
16 4U 1700+24 256.6316 23.9071 256.110961 23.972677 252.098688 46.519124 45.07419011 32.98144858 280.149 54334.7787615741 2007-08-22 18:41:25 54335.875162037 2007-08-23 21:00:14 402023010 50.2445 50 50.2525 50.2605 0 50.2445 2 2 0 2 1 0 0 45.3268 45.3268 94.7158 2 PROCESSED 57539.6636226852 2016-05-31 15:55:37 54723 2008-09-14 00:00:00 54350.4606481482 2007-09-07 11:03:20 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 020105 We propose the observation of Neutron Star Low Mass X-ray Binary (LMXB) system 4U 1700+24.This system would be Advection Dominant Accretion Flow (ADAF) and we research the hard-tail in hard X-ray region. Though the X-ray intensity in a Low Hard state is very faint, $sim$10$^{33}$ erg/s we can obtain the energy spectrum of 10-100keV for the first time using Suzaku 50ksec observation because it is the nearest LMXB. If we know the extension of hard-tail in low luminosity state, we can understand the physical state of electron in the accretion disk and/or compact object. Suzaku is the best satellite to research the faint emission around 100keV. GALACTIC POINT SOURCES 4 B OSAMU NAGAE JAP 2 AO2 STUDY OF MASS ACCRETION FLOW IN ADAF FOR LOW LUMINOUS X-RAY BINARY 4U 1700+24 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402023010/ Quick Look
17 CYG OB2 ASSOCIATION 308.2175 41.2935 307.768848 41.122144 329.008943 57.17316 80.16491027 0.83267098 220.3949 54452.9185532407 2007-12-18 22:02:43 54453.843912037 2007-12-19 20:15:14 402030010 41.1147 40 41.1147 41.1147 0 41.1147 2 2 0 2 1 0 0 37.9181 37.9181 79.9439 0 PROCESSED 57540.9006597222 2016-06-01 21:36:57 54828 2008-12-28 00:00:00 54460.6521643518 2007-12-26 15:39:07 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 020150 Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku. GALACTIC POINT SOURCES 4 C SHUNJI KITAMOTO JAP 2 AO2 STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402030010/ Quick Look
18 EV LAC 341.7127 44.3232 341.158134 44.059332 6.045133 46.919235 100.60502245 -13.08073089 256.1601 54432.9692013889 2007-11-28 23:15:39 54434.4655208333 2007-11-30 11:10:21 402032010 68.9493 100 68.9493 69.1333 0 69.1275 2 1 0 2 1 0 0 65.0113 65.0113 129.2328 2 PROCESSED 57540.7939236111 2016-06-01 19:03:15 54808 2008-12-08 00:00:00 54441.0876851852 2007-12-07 02:06:16 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 021013 We propose a 100 ks Suzaku XIS observation of the dMe flare star EV Lac to measure coronal element abundances during quiescence and flares of different sizes. EV Lac undergoes frequent small flares, and is known to have undergone a very large flare at ~300 times the quiescent count rate in 2000. Coronal abundance changes shed light on the process of chromospheric evaporation under conditions different to those on the Sun. Depending on the size and spectrum of the flare, we may also be able to detect a hard burst of emission that would serve as a time marker for particle acceleration during the flare. GALACTIC POINT SOURCES 4 C UNA HWANG USA 2 AO2 FLARE AND QUIESENT CONORAL ELEMENT ABUNDANCES IN EV LAC XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402032010/ Quick Look
19 VY AQR 318.0426 -8.8307 317.372404 -9.036659 317.753092 7.00586 41.59091784 -35.22055705 252.6652 54414.6528587963 2007-11-10 15:40:07 54415.3855787037 2007-11-11 09:15:14 402043010 25.4473 20 25.4473 25.4473 0 25.4473 2 2 0 2 1 0 0 22.3605 22.3605 63.2999 2 PROCESSED 57540.476712963 2016-06-01 11:26:28 54790 2008-11-20 00:00:00 54423.1702314815 2007-11-19 04:05:08 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 021105 Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. GALACTIC POINT SOURCES 4 C KOJI MUKAI USA 2 AO2 BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402043010/ Quick Look
20 4U1705-44 257.2229 -44.1035 256.319735 -44.039768 260.189733 -21.095668 343.31790137 -2.34044351 107.4157 54543.8610532407 2008-03-18 20:39:55 54544.5210532407 2008-03-19 12:30:19 402051040 20.0744 15 20.0744 20.0744 0 20.0824 2 1 0 2 1 0 0 13.4113 13.4113 57.0179 1 PROCESSED 57541.899525463 2016-06-02 21:35:19 54922 2009-04-01 00:00:00 54553.1912268518 2008-03-28 04:35:22 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 021113 We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. GALACTIC POINT SOURCES 4 A RONALD REMILLARD USA 2 AO2 X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402051040/ Quick Look
21 2S 0921-630 140.6655 -63.298 140.375275 -63.083061 195.139147 -68.890832 281.84446964 -9.33525426 8.3442 54335.887025463 2007-08-23 21:17:19 54336.9932175926 2007-08-24 23:50:14 402059010 43.131 40 43.131 43.131 0 43.131 2 2 0 2 1 0 0 37.1622 37.1622 95.5598 0 PROCESSED 57539.6661805556 2016-05-31 15:59:18 54721 2008-09-12 00:00:00 54350.5504861111 2007-09-07 13:12:42 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 021118 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. GALACTIC POINT SOURCES 4 A JEAN COTTAM USA 2 AO2 PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402059010/ Quick Look
22 2S 0921-630 140.666 -63.2982 140.375774 -63.08326 195.139946 -68.890744 281.84477381 -9.33523447 8.344 54338.0511226852 2007-08-26 01:13:37 54339.16 2007-08-27 03:50:24 402060010 40.3423 40 40.3503 40.3423 0 40.3503 1 1 0 1 1 0 0 35.6464 35.6464 95.7999 2 PROCESSED 57539.6728703704 2016-05-31 16:08:56 54721 2008-09-12 00:00:00 54350.5629398148 2007-09-07 13:30:38 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 021118 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. GALACTIC POINT SOURCES 4 A JEAN COTTAM USA 2 AO2 PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402060010/ Quick Look
23 IGR J17391-3021 264.795 -30.3419 263.992133 -30.314694 265.466386 -6.982553 358.06793122 0.44854091 89.216 54518.4950115741 2008-02-22 11:52:49 54519.3961226852 2008-02-23 09:30:25 402066010 36.4657 30 36.5457 36.5937 0 36.4657 2 2 0 2 1 0 0 31.2591 31.2591 77.8198 1 PROCESSED 57541.7105671296 2016-06-02 17:03:13 54892 2009-03-02 00:00:00 54525.5064699074 2008-02-29 12:09:19 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 021122 We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. GALACTIC POINT SOURCES 4 B JOHN TOMSICK USA 2 AO2 LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402066010/ Quick Look
24 CIRCINUS X-1 230.1633 -57.1695 229.194668 -56.989293 244.120639 -37.250007 322.11384942 0.03740334 115.206 54530.1953240741 2008-03-05 04:41:16 54531.5523032407 2008-03-06 13:15:19 402070010 46.4113 43 46.4113 46.4113 0 46.4113 2 2 0 2 1 0 0 41.8213 41.8213 117.196 0 PROCESSED 57541.8053125 2016-06-02 19:19:39 54916 2009-03-26 00:00:00 54550.2459953704 2008-03-25 05:54:14 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 021128 We propose a 100ks Suzaku observation of Circinus X-1 through the zero (dipping) phase to facilitate 2 important and independent science goals. (1) For the binary, we wish to better understand the viewing geometry, and investigate physical changes in the binary behavior as it relates to observed spectral changes through periastron passage. (2) Conduct a large angle scattering study of the X-ray halo surrounding Circinus X-1 to diagnose ISM grain properties (the line-of-sight position, size distribution, and grain density) near us, in complement with our Chandra halo studies at small angles on grain properties near the source. GALACTIC POINT SOURCES 4 A JULIA LEE USA 2 AO2 CIRCINUS X-1 NEAR PERIASTRON: PROBING BINARY PHYSICS AND ISM GRAINS ALONG THE LINE OF SIGHT XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402070010/ Quick Look
25 CYG X-1 299.5451 35.2618 299.075532 35.125519 313.637974 54.318601 71.3671857 3.12971485 59.9371 54237.8204050926 2007-05-17 19:41:23 54238.6480787037 2007-05-18 15:33:14 402072020 33.3568 30 33.3568 33.3649 0 33.3568 2 1 0 2 1 0 0 32.5637 32.5637 71.5039 1 PROCESSED 57538.696724537 2016-05-30 16:43:17 54695 2008-08-17 00:00:00 54245.0149884259 2007-05-25 00:21:35 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 021133 We request two additional 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. GALACTIC POINT SOURCES 4 A MICHAEL NOWAK USA 2 AO2 CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402072020/ Quick Look
26 1E 1048.1-5937 162.5452 -59.8394 162.049535 -59.57411 203.219635 -58.558248 288.24102095 -0.47209541 101.4368 54800.9597337963 2008-11-30 23:02:01 54802.5927083333 2008-12-02 14:13:30 403005010 100.4231 100 100.443 100.4231 0 100.4231 2 2 0 2 1 0 0 68.1049 68.1049 141.0819 0 PROCESSED 57544.6078472222 2016-06-05 14:35:18 55178 2009-12-13 00:00:00 54812.0471875 2008-12-12 01:07:57 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030013 Observations in soft X-ray through hard X-ray bands are key to understand the emission processes in the magnetosphere of Anomalous X-ray Pulsars (AXPs). We propose to observe the two AXPs, 1E 2259+586 and 1E 1048.1-5937, with SUZAKU. Although no detections of the hard X-ray emissions have been reported, the results of the simulation using XSPEC for HXD indicate that SUZAKU detects the hard X-ray emissions above 20~keV from both AXPs for the first time with a quite high probability. The time resolution of HXD is able to provide the pulse profiles and the phase-resolved spectra in hard X-rays emissions. With these results of the observations, SUZAKU will provide a crucial information to study the emission processes in the magnetosphere of AXPs. GALACTIC POINT SOURCES 4 C JUMPEI TAKATA JAP 3 AO3 X-RAY OBSERVATIONS OF ANOMALOUS X-RAY PULSARS WITH SUZAKU HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403005010/ Quick Look
27 MARS-P3 102.9612 25.1565 102.192848 25.217116 101.724463 2.241555 190.28784034 11.26022306 298.032 54559.4933796296 2008-04-03 11:50:28 54559.5766087963 2008-04-03 13:50:19 403006030 3.886 100 3.886 3.91 0 3.894 1 1 0 1 1 0 0 3.1134 3.1134 7.1839 0 PROCESSED 57542.0373148148 2016-06-03 00:53:44 54953 2009-05-02 00:00:00 54577.0484259259 2008-04-21 01:09:44 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006030/ Quick Look
28 MARS-P11 103.2936 25.1207 102.525618 25.182892 102.027614 2.233108 190.44969799 11.5184009 298.1493 54560.1601041667 2008-04-04 03:50:33 54560.2433333333 2008-04-04 05:50:24 403006110 4.6198 100 4.6278 4.6198 0 4.6358 1 1 0 1 1 0 0 4.0749 4.0749 7.1839 0 PROCESSED 57542.0559490741 2016-06-03 01:20:34 54953 2009-05-02 00:00:00 54577.1745023148 2008-04-21 04:11:17 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006110/ Quick Look
29 MARS-P13 103.3779 25.1101 102.610021 25.172691 102.104653 2.229561 190.49210676 11.58330245 298.1799 54560.3267708333 2008-04-04 07:50:33 54560.41 2008-04-04 09:50:24 403006130 4.2518 100 4.2678 4.2518 0 4.2678 1 1 0 1 1 0 0 3.529 3.529 7.1839 0 PROCESSED 57542.0605671296 2016-06-03 01:27:13 54953 2009-05-02 00:00:00 54577.9292939815 2008-04-21 22:18:11 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006130/ Quick Look
30 MARS-P16 103.503 25.0968 102.735261 25.159983 102.218767 2.2268 190.55275085 11.68067717 298.2223 54560.5768171296 2008-04-04 13:50:37 54560.66 2008-04-04 15:50:24 403006160 2.3262 100 2.3262 2.3262 0 2.3262 2 2 0 2 1 0 0 2.134 2.134 7.1799 0 PROCESSED 57542.0664236111 2016-06-03 01:35:39 54953 2009-05-02 00:00:00 54577.9478935185 2008-04-21 22:44:58 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006160/ Quick Look
31 MARS-P21 103.7101 25.0688 102.942627 25.132964 102.408276 2.21649 190.65860601 11.8395058 298.2947 54560.9933217593 2008-04-04 23:50:23 54561.0765509259 2008-04-05 01:50:14 403006210 2.8808 100 2.8808 2.8808 0 2.8808 1 1 0 1 1 0 0 3.4516 3.4516 7.1839 0 PROCESSED 57542.0774884259 2016-06-03 01:51:35 54953 2009-05-02 00:00:00 54578.0612847222 2008-04-22 01:28:15 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006210/ Quick Look
32 MARS-P23 103.7955 25.0599 103.028122 25.124467 102.486187 2.214951 190.69976585 11.90614711 298.325 54561.1600347222 2008-04-05 03:50:27 54561.2432175926 2008-04-05 05:50:14 403006230 4.5188 100 4.5268 4.5188 0 4.5348 1 1 0 1 1 0 0 3.6868 3.6868 7.1839 0 PROCESSED 57542.0791898148 2016-06-03 01:54:02 54953 2009-05-02 00:00:00 54578.1176157407 2008-04-22 02:49:22 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006230/ Quick Look
33 MARS-P25 103.8803 25.0503 103.113021 25.115268 102.56363 2.212708 190.74132534 11.97202775 298.3546 54561.3266550926 2008-04-05 07:50:23 54561.4098842593 2008-04-05 09:50:14 403006250 4.2612 100 4.2692 4.2612 0 4.2692 1 1 0 1 1 0 0 3.2511 3.2511 7.1839 0 PROCESSED 57542.2336458333 2016-06-03 05:36:27 54953 2009-05-02 00:00:00 54578.1323032407 2008-04-22 03:10:31 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006250/ Quick Look
34 MARS-P26 103.921 25.0474 103.153759 25.112561 102.600638 2.213348 190.75967691 12.00436516 298.3671 54561.4100347222 2008-04-05 09:50:27 54561.4932175926 2008-04-05 11:50:14 403006260 4.7976 100 4.8136 4.7976 0 4.8216 1 1 0 1 1 0 0 3.7622 3.7622 7.1839 0 PROCESSED 57542.2337962963 2016-06-03 05:36:40 54953 2009-05-02 00:00:00 54578.1374074074 2008-04-22 03:17:52 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006260/ Quick Look
35 ARCHES CLUSTER 266.4808 -28.778 265.687528 -28.758983 266.892731 -5.374834 0.16960578 0.02569084 109.9998 54911.0857407407 2009-03-21 02:03:28 54913.7681712963 2009-03-23 18:26:10 403009010 110.7933 100 110.7933 110.7933 0 110.7933 2 2 0 2 1 0 0 91.6578 91.6578 231.7417 3 PROCESSED 57545.9555787037 2016-06-06 22:56:02 55330 2010-05-14 00:00:00 54924.3822106482 2009-04-03 09:10:23 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030029 We propose to observe a hard X-ray ring which has an emission line around 6.4 keV, located at the north of the Arches cluster. The ring is probably produced by an energetic jet or a supernova explosion. We aim to determine the continuum shape, the center energy of the emission line, and the absorption column to figure out the origin of the ring. GALACTIC POINT SOURCES 4 B MASAHIRO TSUJIMOTO JAP 3 AO3 A 6.4 KEV RING AT THE NORTH OF THE ARCHES CLUSTER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403009010/ Quick Look
36 LS I+61 303_1 40.1455 61.188 39.183267 60.973753 59.828193 42.868734 135.69810374 1.0510579 270.0003 54853.9515856482 2009-01-22 22:50:17 54854.8648032407 2009-01-23 20:45:19 403015010 40.5514 40 40.5514 40.5514 0 40.5514 2 2 0 2 1 0 0 25.7312 25.7312 78.868 0 PROCESSED 57545.3022916667 2016-06-06 07:15:18 55329 2010-05-13 00:00:00 54880.5343865741 2009-02-18 12:49:31 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030077 We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. GALACTIC POINT SOURCES 4 A YASUSHI FUKAZAWA JAP 3 AO3 X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403015010/ Quick Look
37 LS I+61 303_2 40.1457 61.1877 39.18347 60.973453 59.828143 42.868421 135.69831419 1.05082335 270.0006 54856.6966087963 2009-01-25 16:43:07 54858.1766666667 2009-01-27 04:14:24 403016010 61.0667 60 61.0784 61.0667 0 61.0784 2 2 0 2 1 0 0 26.6591 26.6591 127.8398 1 PROCESSED 57545.3828819444 2016-06-06 09:11:21 55329 2010-05-13 00:00:00 54880.5522106482 2009-02-18 13:15:11 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030077 We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. GALACTIC POINT SOURCES 4 A YASUSHI FUKAZAWA JAP 3 AO3 X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403016010/ Quick Look
38 LS I+61 303_3 40.2018 61.1949 39.239095 60.980826 59.865781 42.86376 135.72005286 1.06843757 246.2753 54872.1842592593 2009-02-10 04:25:20 54873.7252199074 2009-02-11 17:24:19 403017010 68.6273 60 68.6273 68.6273 0 68.6273 2 2 0 2 1 0 0 65.0685 65.0685 133.1218 1 PROCESSED 57545.5290856482 2016-06-06 12:41:53 55330 2010-05-14 00:00:00 54893.4210300926 2009-03-03 10:06:17 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030077 We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. GALACTIC POINT SOURCES 4 A YASUSHI FUKAZAWA JAP 3 AO3 X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403017010/ Quick Look
39 IGR J16194-2810 244.8908 -28.0663 244.116394 -27.946439 247.849887 -6.534784 349.1669856 15.58223604 95.1879 54867.1762152778 2009-02-05 04:13:45 54868.4314236111 2009-02-06 10:21:15 403024010 45.5687 50 45.5687 45.5738 0 45.5687 2 2 0 2 1 0 0 38.7859 38.7859 108.4358 1 PROCESSED 57545.4895023148 2016-06-06 11:44:53 55329 2010-05-13 00:00:00 54880.5743518518 2009-02-18 13:47:04 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030121 We propose to observe the weakly magnetized neutron star X-ray binary, IGR J16194-2810. This target object has almost constant luminosity and is expected to be state of ADAF. Assuming that we observe the object using HXD and XIS of the Suzaku for 50ks, we can investigate the soft X-ray emission from the NS and/or the accretion disk and hard X-ray tail. Comparing Black Body and Disk Black Body parameters of this object with that of fainter source, 4U 1700+24, we obtain a picture of accretion disk and accretion flow. If we measure the photon index and cutoff energy of the hard tail, we can reveal the physical condition of corona surrounding the NS or the disk. Only Suzaku can carry out this observation which observe soft-thermal and hard-nonthermal X-ray emission from faint source. GALACTIC POINT SOURCES 4 C OSAMU NAGAE JAP 3 AO3 ELUCIDATION OF THE ADAF OBSERVING LOW LUMINOUS NEUTRON STAR X-RAY BINARY IGR J16194-2810 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403024010/ Quick Look
40 V709 CAS 7.1951 59.3013 6.498819 59.024957 38.349683 49.774418 120.03837674 -3.44309479 84.0816 54637.4334837963 2008-06-20 10:24:13 54638.1542824074 2008-06-21 03:42:10 403025010 35.8982 30 35.8982 35.8982 0 35.8982 2 2 0 2 1 0 0 33.3823 33.3823 62.2679 0 PROCESSED 57542.8811921296 2016-06-03 21:08:55 55014 2009-07-02 00:00:00 54648.3358101852 2008-07-01 08:03:34 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030140 Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. GALACTIC POINT SOURCES 4 B KEN EBISAWA JAP 3 AO3 IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403025010/ Quick Look
41 RX J1940.1-1025 295.0445 -10.4193 294.356962 -10.535652 295.074294 10.867465 28.98688715 -15.49869645 79.7405 54572.8979976852 2008-04-16 21:33:07 54573.743275463 2008-04-17 17:50:19 403027010 32.4536 30 32.4536 32.4536 0 32.4536 2 2 0 2 1 0 0 26.4657 26.4657 73.0219 2 PROCESSED 57542.3241087963 2016-06-03 07:46:43 54953 2009-05-02 00:00:00 54587.0481481482 2008-05-01 01:09:20 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030140 Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. GALACTIC POINT SOURCES 4 B KEN EBISAWA JAP 3 AO3 IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403027010/ Quick Look
42 TAU SCO 248.9736 -28.2151 248.194076 -28.113426 251.450456 -6.117318 351.53721955 12.80675658 279.3712 54723.4207291667 2008-09-14 10:05:51 54723.8119675926 2008-09-14 19:29:14 403034030 12.2902 10 12.2982 12.2982 0 12.2902 1 1 0 1 1 0 0 11.0282 11.0282 33.7999 0 PROCESSED 57543.8133564815 2016-06-04 19:31:14 55148 2009-11-13 00:00:00 54780.4631597222 2008-11-10 11:06:57 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 031121 We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. GALACTIC POINT SOURCES 4 A RICHARD IGNACE USA 3 AO3 X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403034030/ Quick Look
43 ETA CARINAE 161.2297 -59.7314 160.743721 -59.468116 202.194195 -58.967017 287.60304523 -0.67930865 294 54627.0775 2008-06-10 01:51:36 54627.649525463 2008-06-10 15:35:19 403035010 35.4479 30 35.4639 35.4479 0 35.4639 2 2 0 2 1 0 0 27.2102 27.2102 49.4159 1 PROCESSED 57542.7628819445 2016-06-03 18:18:33 55003 2009-06-21 00:00:00 54637.2680092593 2008-06-20 06:25:56 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 031124 X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). GALACTIC POINT SOURCES 4 A KENJI HAMAGUCHI USA 3 AO3 X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403035010/ Quick Look
44 ETA CARINAE 161.3639 -59.6742 160.876523 -59.410706 202.202933 -58.878505 287.63630523 -0.59715454 170.6228 54877.528287037 2009-02-15 12:40:44 54878.4119675926 2009-02-16 09:53:14 403038010 35.5525 30 35.5685 35.5525 0 35.5605 2 2 0 2 1 0 0 31.1193 31.1193 76.3239 1 PROCESSED 57545.5564814815 2016-06-06 13:21:20 55328 2010-05-12 00:00:00 54893.4307407407 2009-03-03 10:20:16 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 031124 X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). GALACTIC POINT SOURCES 4 A KENJI HAMAGUCHI USA 3 AO3 X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403038010/ Quick Look
45 SS73 17 152.7399 -57.7545 152.30201 -57.507445 193.309145 -60.825813 282.81739372 -1.29143094 80.1552 54775.6877430556 2008-11-05 16:30:21 54776.3072453704 2008-11-06 07:22:26 403043010 24.907 20 24.907 24.907 0 24.907 2 2 0 2 1 0 0 20.8091 20.8091 53.5199 0 PROCESSED 57544.3629282407 2016-06-05 08:42:37 55157 2009-11-22 00:00:00 54791.6362847222 2008-11-21 15:16:15 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 031145 SS73 17 was an innocuous Mira-type symbiotic star until INTEGRAL and Swift discovered its bright hard X-ray emission. Suzaku observations showed it emits three bright iron lines, with almost no emission in the 0.5-2 keV bandpass. The PI has an approved 100 ksec Chandra HETG observation in 2008 to determine the origin of the iron lines and measure any weak emission lines. With simultaneous Suzaku observations we will also measure the hard X-ray emission from the source, both to constrain the continuum and detect any non-thermal component. The effective areas of the XIS and HXD will constrain the broadband emission process much better than the HETG data. Combined with simultaneous optical observations of the Mira-type star we will determine the origin of this star's unusual emission. GALACTIC POINT SOURCES 4 A RANDALL SMITH USA 3 AO3 SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS OF THE SYMBIOTIC STAR SS73 17 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403043010/ Quick Look
46 1A1118-61 170.3215 -61.8847 169.770459 -61.610411 210.906306 -57.212373 292.5244731 -0.84831529 142.606 54859.2344328704 2009-01-28 05:37:35 54859.8925810185 2009-01-28 21:25:19 403050010 44.2125 45 44.2125 44.2125 0 44.2125 2 2 0 2 1 0 0 30.9154 30.9154 56.8599 0 PROCESSED 57545.3633680556 2016-06-06 08:43:15 55328 2010-05-12 00:00:00 54880.5326273148 2009-02-18 12:46:59 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 031155 We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku AO3. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line in this system and to determine its broad band spectrum. GALACTIC POINT SOURCES 4 A KATJA POTTSCHMIDT USA 3 AO3-TOO SEARCHING FOR CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403050010/ Quick Look
47 CYG X-1 299.5797 35.2714 299.110135 35.134972 313.689122 54.31814 71.39012673 3.11059703 84.4565 54574.6816898148 2008-04-18 16:21:38 54575.4238425926 2008-04-19 10:10:20 403065010 33.9435 30 33.9435 33.9782 0 33.9703 1 1 0 2 1 0 0 28.9556 28.9556 64.118 0 PROCESSED 57542.3725231482 2016-06-03 08:56:26 54957 2009-05-06 00:00:00 54587.2117476852 2008-05-01 05:04:55 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 031172 We request two 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku brings three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 100-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. GALACTIC POINT SOURCES 4 A MICHAEL NOWAK USA 3 AO3 CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN IN THE SUZAKU ERA HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403065010/ Quick Look
48 GS 1826-238 277.3735 -23.8572 276.610421 -23.891095 276.73109 -0.588705 9.22092987 -6.12003001 267.2862 55125.8488310185 2009-10-21 20:22:19 55127.9502777778 2009-10-23 22:48:24 404007010 102.5154 100 102.5154 102.5314 0 102.5372 2 2 0 2 1 0 0 87.9996 87.9996 181.5418 2 PROCESSED 57549.0104976852 2016-06-10 00:15:07 55534 2010-12-04 00:00:00 55166.4220833333 2009-12-01 10:07:48 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 040035 We propose a 100 ksec Suzaku observation of the neutron star (NS) binary GS 1826-238. It is already known that there is a high energy cutoff at around 150 keV in the hard state of black hole candidates (BNCs). Additional non-thermal spectrum above 300 keV has sometimes been verified by gamma-ray observatories. Some NS binaries exhibit a 'hard state' which shows X-ray properties similar to those observed in hard state BHCs. Their cutoff energies (~50 keV) are systematically lower than those of BHCs, but firm detections of non-thermal emissions are not reported so far. This proposal is aimed at the first detection of the non-thermal hard tail from this source in the steady 'hard state', and verification of its possible jet origin via simultaneous radio, near-IR, and optical observations. GALACTIC POINT SOURCES 4 B KAZUTAKA YAMAOKA JAP 4 AO4 SEARCH FOR A NON-THERMAL HARD TAIL FROM THE NEUTRON STAR BINARY GS 1826-238 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404007010/ Quick Look
49 EUVE J0317-85.5 48.9864 -85.5003 51.11405 -85.679196 278.533864 -69.749958 299.84736337 -30.72881529 65.46 55028.6017476852 2009-07-16 14:26:31 55030.1460185185 2009-07-18 03:30:16 404019010 63.0843 60 63.0843 63.0843 0 63.0843 2 2 0 2 1 0 0 56.8965 56.8965 133.4138 1 PROCESSED 57547.8712847222 2016-06-08 20:54:39 55406 2010-07-29 00:00:00 55040.2674305556 2009-07-28 06:25:06 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 040083 Where is the particle acceleration site in the universe? The Cosmic-ray origin is the long standing mystery for near 100 years. The first discovery of "the white dwarf pulsar" in the AE Aquarii system with Suzaku is one of the most important step in this study, because Suzaku demonstrated the possibility of particle acceleration in white dwarfs. The next important step is to search for the sign of non-thermal emission from a NORMAL white dwarf. Here, we propose the Suzaku observation of an isolated white dwarf EUVE J0317-85.5, which has very high magnetic field strength of 450 MG and very fast rotation period 725 sec among this type of objects. GALACTIC POINT SOURCES 4 B ATSUSHI HARAYAMA JAP 4 AO4 FIRST SEARCH FOR NON THERMAL EMISSION FROM AN ISOLATED MAGNETIZED WHITE DWARF HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404019010/ Quick Look
50 TT ARI 31.7181 15.2972 31.038138 15.059527 34.795947 2.311089 148.52228749 -43.79443 71.0668 55018.4424652778 2009-07-06 10:37:09 55019.3023611111 2009-07-07 07:15:24 404021010 35.7421 35 35.7421 35.7796 0 35.7876 2 2 0 2 1 0 0 31.794 31.794 74.2578 1 PROCESSED 57547.7822453704 2016-06-08 18:46:26 55399 2010-07-22 00:00:00 55029.236712963 2009-07-17 05:40:52 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 040095 The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail. GALACTIC POINT SOURCES 4 B KEI SAITOU JAP 4 AO4 IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404021010/ Quick Look
51 TX COL 85.7822 -41.0648 85.383592 -41.086265 82.635964 -64.399356 246.79781267 -29.77494364 322.4827 54963.6800578704 2009-05-12 16:19:17 54965.2502199074 2009-05-14 06:00:19 404031010 59.7818 40 59.7898 59.7898 0 59.7818 2 2 0 2 1 0 0 51.123 51.123 135.654 0 PROCESSED 57546.5734143518 2016-06-07 13:45:43 55345 2010-05-29 00:00:00 54978.2105439815 2009-05-27 05:03:11 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 040113 We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. GALACTIC POINT SOURCES 4 A TAKAYUKI YUASA JAP 4 AO4 SURVEY OBSERVATION OF INTERMEDIATE POLARS HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404031010/ Quick Look
52 V773 TAU 63.5591 28.1916 62.7857 28.065974 66.717215 6.863448 168.22897578 -16.34488481 264.3183 55255.9666550926 2010-02-28 23:11:59 55258.750162037 2010-03-03 18:00:14 404037010 115.4057 120 115.4057 115.4057 0 115.4057 2 2 0 2 1 0 0 95.563 95.563 240.4667 1 PROCESSED 57550.8499189815 2016-06-11 20:23:53 55637 2011-03-17 00:00:00 55271.499537037 2010-03-16 11:59:20 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 041203 Young stars display magnetic activity at the extreme of that produced in nearby active stars and the Sun, making them useful tools to probe the dominant physical processes controlling such activity. The unique features of V773 Tau's X-ray and radio properties (frequent X-ray flaring of highly energetic flares, extreme nonthermal radio emission) mark it as one of the most active young stars. We seek coordinated Suzaku and mm wavelength observations to probe the interplay between the hot plasma and the stellar environment. We focus on utilizing the unique capabilities of Suzaku, namely the spectral resolution and sensitivity at 5--10 keV, to elucidate the properties of its hot plasma and its potential effects on the stellar environment such as detecting Fe fluorescence. GALACTIC POINT SOURCES 4 C RACHEL OSTEN USA 4 AO4 X-RAY EMISSION AND THE STELLAR ENVIRONMENT AROUND THE PRE-MAIN SEQUENCE BINARY V773 TAU XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404037010/ Quick Look
53 ETA CARINAE 161.2575 -59.6351 160.770713 -59.371773 202.076586 -58.890955 287.57052339 -0.58758586 87.8919 55156.1883449074 2009-11-21 04:31:13 55157.3196643518 2009-11-22 07:40:19 404039010 49.3887 45 49.3887 49.3887 0 49.3887 2 2 0 2 1 0 0 34.2553 34.2553 97.7201 0 PROCESSED 57549.5287152778 2016-06-10 12:41:21 55542 2010-12-12 00:00:00 55176.3651388889 2009-12-11 08:45:48 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 041204 The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements. GALACTIC POINT SOURCES 4 A KENJI HAMAGUCHI USA 4 AO4 HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CAR HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404039010/ Quick Look
54 GRS 1758-258 270.2971 -25.679 269.522467 -25.678561 270.258372 -2.238361 4.56169204 -1.32563061 89.3817 55263.8983333333 2010-03-08 21:33:36 55266.0711111111 2010-03-11 01:42:24 404060010 82.6827 80 82.6827 82.6827 0 82.6827 2 2 0 2 1 0 0 71.1789 71.1789 187.7097 1 PROCESSED 57550.8664583333 2016-06-11 20:47:42 55647 2011-03-27 00:00:00 55279.5468402778 2010-03-24 13:07:27 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 041244 We propose an 80 ks observation to obtain a broadband spectrum of the Galactic microquasar GRS 1758-258 while in the low-hard state with Suzaku. Here we aim to constrain the nature and geometry of the accretion flow via measurements of the various disc reflection features, which are detectable for the first time due to the unique capabilities of Suzaku. As this system is known to power large radio jets, its study will also aid our understanding of the conditions necessary for the formation of relativistic outflows and how these relate to the accretion geometry in the low-hard state. GALACTIC POINT SOURCES 4 B MARK REYNOLDS USA 4 AO4 CONSTRAINING DISC REFLECTION IN THE MICROQUASAR GRS 1758-258 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404060010/ Quick Look
55 LMC X-1 84.947 -69.7479 85.058791 -69.772179 298.110491 -86.30257 280.20680376 -31.50316575 10.0004 55033.776724537 2009-07-21 18:38:29 55036.8953587963 2009-07-24 21:29:19 404061010 129.8679 120 129.8679 129.8679 0 129.8679 2 2 0 2 1 0 0 132.5976 132.5976 269.3956 4 PROCESSED 57548.0199537037 2016-06-09 00:28:44 55419 2010-08-11 00:00:00 55048.6509143518 2009-08-05 15:37:19 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 041245 We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability. GALACTIC POINT SOURCES 4 A JEFFREY MCCLINTOCK USA 4 AO4 MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404061010/ Quick Look
56 LMC X-3 84.7128 -64.0821 84.643099 -64.107952 45.920225 -86.688866 273.5746003 -32.09166858 184.4521 55186.5265162037 2009-12-21 12:38:11 55190.9105555556 2009-12-25 21:51:12 404062010 154.4242 150 154.434 154.434 0 154.4242 2 2 0 2 1 0 0 101.1721 101.1721 352.1458 2 PROCESSED 57550.1364930556 2016-06-11 03:16:33 55587 2011-01-26 00:00:00 55218.7384375 2010-01-22 17:43:21 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 041245 We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability. GALACTIC POINT SOURCES 4 C JEFFREY MCCLINTOCK USA 4 AO4 MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404062010/ Quick Look
57 4U 1820-30 275.9251 -30.4172 275.121541 -30.443999 275.136917 -7.082068 2.74021083 -7.94370371 265.2009 55111.1096643518 2009-10-07 02:37:55 55111.700162037 2009-10-07 16:48:14 404069050 21.7674 20 21.7674 21.7674 0 21.7674 1 1 0 1 1 0 0 15.6743 15.6743 51.0039 0 PROCESSED 57548.7799884259 2016-06-09 18:43:11 55496 2010-10-27 00:00:00 55127.2938194445 2009-10-23 07:03:06 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A MANUEL LINARES EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069050/ Quick Look
58 GX 9+9 262.9404 -16.8929 262.215892 -16.856936 263.194726 6.381396 8.57505694 9.06920034 97.5329 55271.6738773148 2010-03-16 16:10:23 55273.9918981482 2010-03-18 23:48:20 404071010 85.1871 75 85.2087 85.2031 0 85.1871 2 1 0 2 1 0 0 61.6942 61.6942 200.2639 0 PROCESSED 57550.9767476852 2016-06-11 23:26:31 55652 2011-04-01 00:00:00 55285.4179513889 2010-03-30 10:01:51 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 042011 We propose two 75 ks Suzaku observations of the bright neutron star low mass X-ray binary (LMXB) GX9+9, spread over six months. We will investigate the presence of X-ray narrow absorption features in the Suzaku spectra, which are a signature of a disk wind. Such features, identified with ions such as Fe XXV and Fe XXVI, have been observed in a number of LMXBs and give us information about the mass outflow rate and the launching mechanism of the wind. We will study the connection of the disk wind to the presence of radio jet emission with simultaneous radio observations. Finally, we will determine if the broad Fe emission line indicated by the XMM-Newton spectrum is relativistically broadened. Variability will be studied as a function of accretion rate in the two proposed observations. GALACTIC POINT SOURCES 4 B MARIA DIAZ TRIGO EUR 4 AO4 A STUDY OF THE DISK WIND-JET CONNECTION IN GX9+9 WITH MULTIWAVELENGTH OBSERVATIONS HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404071010/ Quick Look
59 CYGNUS X-1 299.5392 35.2589 299.069624 35.122644 313.628523 54.317489 71.36219421 3.13231837 55.3254 54957.7006828704 2009-05-06 16:48:59 54958.1356365741 2009-05-07 03:15:19 404075060 19.4345 300 19.4345 19.4505 0 19.4345 2 1 0 2 1 0 0 15.2795 15.2795 37.5579 0 PROCESSED 57546.5121412037 2016-06-07 12:17:29 54922 2009-04-01 00:00:00 54976.0885300926 2009-05-25 02:07:29 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075060/ Quick Look
60 CYGNUS X-1 299.5373 35.2573 299.067717 35.121052 313.625096 54.316504 71.3600172 3.13281014 53.4895 54976.3582060185 2009-05-25 08:35:49 54976.8259722222 2009-05-25 19:49:24 404075090 20.9252 300 20.9252 20.9332 0 20.9252 2 1 0 2 1 0 0 16.1164 16.1164 40.412 1 PROCESSED 57546.6796296296 2016-06-07 16:18:40 54922 2009-04-01 00:00:00 54992.6651736111 2009-06-10 15:57:51 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075090/ Quick Look
61 CYGNUS X-1 299.5294 35.2515 299.059794 35.115286 313.611339 54.313209 71.35169447 3.13529932 46.7675 54984.481400463 2009-06-02 11:33:13 54984.9870833333 2009-06-02 23:41:24 404075110 17.4502 300 19.037 17.7782 0 17.4502 1 1 0 1 1 0 0 15.0409 15.0409 43.6879 1 PROCESSED 57547.4475462963 2016-06-08 10:44:28 54922 2009-04-01 00:00:00 54994.4091087963 2009-06-12 09:49:07 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075110/ Quick Look
62 CYGNUS X-1 299.6354 35.1397 299.164908 35.003038 313.686688 54.178801 71.30132058 3.00311627 241.1557 55159.514224537 2009-11-24 12:20:29 55160.1328587963 2009-11-25 03:11:19 404075180 21.7685 300 21.7685 22.4805 0 22.4725 5 2 0 3 1 0 0 11.4064 11.4064 53.4358 0 PROCESSED 57549.5783680556 2016-06-10 13:52:51 54922 2009-04-01 00:00:00 55176.294849537 2009-12-11 07:04:35 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A JON MILLER SHIN YAMADA USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075180/ Quick Look
63 4U0142+61 26.5176 61.8112 25.649771 61.561225 52.160955 46.451759 129.33625727 -0.37933599 61.041 55055.0703125 2009-08-12 01:41:15 55057.3654976852 2009-08-14 08:46:19 404079010 107.4129 100 107.4129 107.4209 0 107.4227 2 2 0 2 1 0 0 99.7576 99.7576 198.2838 2 PROCESSED 57548.2012152778 2016-06-09 04:49:45 54922 2009-04-01 00:00:00 55068.3037268518 2009-08-25 07:17:22 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A KAZUO MAKISHIMA JAP 4 AO4 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404079010/ Quick Look
64 PSR J1846-0258 281.5972 -2.9106 280.942424 -2.965017 282.329422 20.034924 29.7662115 -0.20474108 86.0001 54936.8175578704 2009-04-15 19:37:17 54939.6779398148 2009-04-18 16:16:14 404081010 104.3451 100 104.3451 104.3675 0 104.3531 2 2 0 2 1 0 0 76.0065 76.0065 247.1018 1 PROCESSED 57546.2746990741 2016-06-07 06:35:34 54922 2009-04-01 00:00:00 54959.5006018518 2009-05-08 12:00:52 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A KAZUO MAKISHIMA JAP 4 AO4 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404081010/ Quick Look
65 V773TAU 63.5571 28.1952 62.783682 28.069565 66.716115 6.867305 168.22500409 -16.34364304 260.6557 55610.1581712963 2011-02-18 03:47:46 55611.9815277778 2011-02-19 23:33:24 405011010 82.2463 80 82.2543 82.2463 0 82.2543 2 2 0 2 1 0 0 72.8287 72.8287 157.5258 2 PROCESSED 57601.0256134259 2016-08-01 00:36:53 55990 2012-03-04 00:00:00 55621.2978703704 2011-03-01 07:08:56 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 050033 We propose a Suzaku observation of the pre-main sequence binary system V773 Tau with the high sensitivity of HXD. The empirical Lx-Lr relation (Benz-G"udel relation) and radio flux variation predict that this source can have a flare with a peak luminosity Lx=10^34 ergs s-1, seven orders of magnitude larger than that of the Sun, when it is just before the periastron passage. We will observe this target simultaneously with radio band using VLBI network. Our goal is (1) to test whether the gigantic flare is still on the empirical relation (2) to detect inpulsive non-thermal emission at the most powerful stellar flare (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band. GALACTIC POINT SOURCES 4 B YOHKO TSUBOI JAP 5 AO5 NON-THERMAL EMISSION AT THE MOST POWERFUL STELLAR FLARE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405011010/ Quick Look
66 1E 1547.0-5408 237.7284 -54.3676 236.761869 -54.21692 248.127922 -33.347549 327.20000551 -0.18012949 271.1663 55415.1611921296 2010-08-07 03:52:07 55415.9633796296 2010-08-07 23:07:16 405024010 51.6728 50 51.6728 51.7928 0 52.1529 2 2 0 1 1 0 0 42.7812 42.7812 69.2999 0 PROCESSED 57552.8870949074 2016-06-13 21:17:25 55793 2011-08-20 00:00:00 55427.247025463 2010-08-19 05:55:43 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 050099 Recently, hard X-ray tails have been detected by INTEGRAL at least up to 150 keV from ~5 magnetars. Suzaku has observed some magnetars during Key Project (AO-4) and ToO observations. As a result, soft X-ray emissions and hard X-ray tails have been detected from ~10 magnetars. This peculiar spectrum is seem to be common in all the magnetars, and we discovered the spectral evolution of magnetars. The remaining problem is to study the spectral difference between the active and quiescent states. Transient magnetar 1E 1547.0-540 was observed with Suzaku in 2009 January, and the extremely hard X-ray tail was detected up to 110 keV with photon index of 1.5, and it is appropriate to study the spectral change. Thus, we propose the observation of 1E 1547.0-5408 with 50 ks. GALACTIC POINT SOURCES 4 B HIROYUKI NISHIOKA JAP 5 AO5 OBSERVATION OF THE HARD X-RAY TAIL AND SOFT X-RAY EMISSION OF AXP 1E 1547.0-5408 IN QUIESCENT STATE HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405024010/ Quick Look
67 EMS1150 263.083 -32.7212 262.264926 -32.685689 264.095488 -9.421504 355.27740066 0.39306698 91.2452 55611.9964930556 2011-02-19 23:54:57 55612.6968055556 2011-02-20 16:43:24 405026010 20.9186 20 20.9186 20.9186 0 20.9186 1 1 0 1 1 0 0 17.2639 17.2639 60.5039 0 PROCESSED 57600.9777893518 2016-07-31 23:28:01 55988 2012-03-02 00:00:00 55621.1440740741 2011-03-01 03:27:28 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 050104 Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. GALACTIC POINT SOURCES 4 A YASUYUKI TANAKA JAP 5 AO5 SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405026010/ Quick Look
68 EG AND 11.168 40.673 10.482613 40.399604 27.902454 32.653699 121.54657283 -22.18054863 225.2111 55597.6281018518 2011-02-05 15:04:28 55600.0030092593 2011-02-08 00:04:20 405034010 100.5333 100 100.5333 100.5413 0 100.5493 2 2 0 2 1 0 0 84.6589 84.6589 205.1719 3 PROCESSED 57600.9241666667 2016-07-31 22:10:48 55983 2012-02-26 00:00:00 55614.2972106482 2011-02-22 07:07:59 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 051211 The goals of this proposal are to use Suzaku XIS observations to : 1) determine whether EG And, BX Mon, and BF Cyg are members of the recently recognized class of hard X-ray emitting symbiotic stars; and 2) if they are, compare the nature of any absorption, the optical depth of the boundary layer, and the accretion rate to those of the well established hard X-ray symbiotics. Understanding the accretion processes in symbiotic stars is a crucial step in determining the role they play as progenitors of type Ia supernovae. GALACTIC POINT SOURCES 4 C THOMAS NELSON USA 5 AO5 EXPLORING THE ACCRETION DISK BOUNDARY LAYERS OF SYMBIOTIC STARS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405034010/ Quick Look
69 4U 1626-67 248.0734 -67.4643 246.814526 -67.35746 258.330198 -44.907314 321.7866399 -13.09493758 285.8172 55445.5409259259 2010-09-06 12:58:56 55446.2376273148 2010-09-07 05:42:11 405044010 20.0335 20 20.0335 20.0575 0 20.0457 2 2 0 2 1 0 0 19.5372 19.5372 60.1799 0 PROCESSED 57553.3082175926 2016-06-14 07:23:50 55822 2011-09-18 00:00:00 55456.2336574074 2010-09-17 05:36:28 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 051234 Recent X-ray observations by Fermi/GBM and Swift/BAT of 4U 1626-67 discovered a new torque reversal of this source after 18 years of steady spinning down. Centered on Feb 4 2008, a dramatic increase in the X-ray flux was also observed. The lack of correlation between the X-ray flux and the torque applied to the neutron star before the transition, challenges our understanding of the physical mechanisms operating in this system. The main goal of this proposal is to look for changes in the long term flux behavior, energy spectra, pulse profile, line features and power spectra with the current evolution in 4U1626-67 s spin-up rate. In addition, we wish to determine whether the absence of the QPO observed just after the torque reversal persist. GALACTIC POINT SOURCES 4 A MARK FINGER USA 5 AO5 THE ACCRETING X-RAY PULSAR 4U 1626-67 AFTER A NEW TORQUE REVERSAL XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405044010/ Quick Look
70 4U 1957+11 299.8589 11.6979 299.267976 11.560536 304.903477 31.592045 51.30303986 -9.34292333 251.3459 55501.8275462963 2010-11-01 19:51:40 55502.7001157407 2010-11-02 16:48:10 405057030 35.3491 35 35.3571 35.3491 0 35.3571 2 2 0 2 1 0 0 27.1697 27.1697 75.362 0 PROCESSED 57553.9520601852 2016-06-14 22:50:58 55881 2011-11-16 00:00:00 55515.3015046296 2010-11-15 07:14:10 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 051254 We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. GALACTIC POINT SOURCES 4 B MICHAEL NOWAK USA 5 AO5 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405057030/ Quick Look
71 HER X-1 254.4632 35.2657 254.012163 35.341297 246.023504 57.418254 58.05457552 37.50615868 268.4858 55461.0002083333 2010-09-22 00:00:18 55461.4494675926 2010-09-22 10:47:14 405058030 19.924 20 19.924 19.924 0 20.2438 2 2 0 1 1 0 0 17.5073 17.5073 38.8119 0 PROCESSED 57553.4994560185 2016-06-14 11:59:13 55836 2011-10-02 00:00:00 55470.1508796296 2010-10-01 03:37:16 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052001 We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? GALACTIC POINT SOURCES 4 B R DIGER STAUBERT EUR 5 AO5 VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405058030/ Quick Look
72 GX 339-4 255.7015 -48.7852 254.753736 -48.714186 259.571673 -25.859287 338.94105133 -4.32146688 83.6944 55603.7634722222 2011-02-11 18:19:24 55604.2349421296 2011-02-12 05:38:19 405063010 22.4594 100 22.4594 22.4594 0 22.4834 2 2 0 2 1 0 0 19.3287 19.3287 40.7279 0 PROCESSED 57600.9244675926 2016-07-31 22:11:14 55983 2012-02-26 00:00:00 55617.4120601852 2011-02-25 09:53:22 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CLEMENT CABANAC EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063010/ Quick Look
73 GX 339-4 255.7013 -48.7848 254.753541 -48.713785 259.571479 -25.858904 338.94128957 -4.32111913 86.3597 55608.9686111111 2011-02-16 23:14:48 55609.6501967593 2011-02-17 15:36:17 405063020 21.0157 20 21.0157 21.0157 0 21.0157 2 2 0 2 1 0 0 17.5958 17.5958 58.8839 0 PROCESSED 57600.9613773148 2016-07-31 23:04:23 55988 2012-03-02 00:00:00 55621.1561342593 2011-03-01 03:44:50 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CLEMENT CABANAC EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063020/ Quick Look
74 GX 339-4 255.7016 -48.7831 254.753859 -48.712086 259.571491 -25.857192 338.94276391 -4.32024293 90.1024 55616.8233680556 2011-02-24 19:45:39 55617.4487268518 2011-02-25 10:46:10 405063030 19.182 20 19.19 19.198 0 19.182 2 2 0 2 1 0 0 15.684 15.684 54.0259 1 PROCESSED 57601.0471180556 2016-08-01 01:07:51 55996 2012-03-10 00:00:00 55628.1679976852 2011-03-08 04:01:55 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CLEMENT CABANAC EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063030/ Quick Look
75 4U1812-12 273.8053 -12.0935 273.104949 -12.110284 273.784611 11.297146 18.04900466 2.37362039 267.159 55838.1400347222 2011-10-04 03:21:39 55839.9168981482 2011-10-05 22:00:20 406008010 62.0143 60 62.0143 62.0143 0 62.0143 2 2 0 2 1 0 0 53.5441 53.5441 153.5099 1 PROCESSED 57603.3255902778 2016-08-03 07:48:51 56226 2012-10-26 00:00:00 55858.3124768518 2011-10-24 07:29:58 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 060012 Low-Mass X-ray binaries (LMXBs) are known to have soft and hard states, like black hole binaries. Through an analysis of archival Suzaku data of the LMXB Aql X-1 in the hard state, we obtained a clear picture of its accretion geometry; a truncated accretion disk, and a hot corona that Comptonize blackbody photons from the neutron star surface. In order to investigate whether this picture also applies to other LMXBs in the low/hard state, and to better constrain the accretion geometry in comparison with those of black hole binaries, we propose a 60 ksec Suzaku observation of the LMXB 4U 1812-12. This is a valuable object,which is known to reside almost always in the low/hard state. GALACTIC POINT SOURCES 4 A SOKI SAKURAI JAP 6 AO6 REVEALING THE ACCRETION GEOMETRY OF THE LOW/HARD STATE LMXB 4U 1812-12 WITH SUZAKU XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406008010/ Quick Look
76 VW HYI 62.3084 -71.2978 62.399199 -71.427045 322.000013 -79.107776 284.88912946 -38.12913625 338.7313 56049.8124305556 2012-05-02 19:29:54 56050.1668171296 2012-05-03 04:00:13 406009040 16.8177 20 16.8257 16.8257 0 16.8177 2 1 0 2 1 0 0 13.9478 13.9478 30.6159 0 PROCESSED 57605.3312847222 2016-08-05 07:57:03 56449 2013-06-06 00:00:00 56083.0857060185 2012-06-05 02:03:25 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 060023 SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. GALACTIC POINT SOURCES 4 B KEI SAITOU JAP 6 AO6-TOO TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009040/ Quick Look
77 CYG X-1 299.5916 35.1745 299.121401 35.038023 313.64901 54.223609 71.31236822 3.05181611 279.5001 55839.9245023148 2011-10-05 22:11:17 55840.9169328704 2011-10-06 22:00:23 406013010 3.7027 40 3.832 3.7027 0 40.2718 1 1 0 1 1 0 0 32.9625 32.9625 85.7339 1 PROCESSED 57603.3954166667 2016-08-03 09:29:24 56582 2013-10-17 00:00:00 56212.7247916667 2012-10-12 17:23:42 3.0.22.44 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 060057 We achieved 0.1 s time resolution with enough statistics on accumulating profiles of source brightening and made clear that electron temperature decreases and optical depth increases at the peak of brightness by using the XIS data of Psum mode. Progress to understanding the nature of fast time variability, which has been a mystery for 40 years since its discovery, connected with spectral properties is being made now. However, this property is not confirmed yet in other observations having different time scales of variability and spectral shapes, lacking the XIS data in Psum mode. We propose here another observation of Cyg X-1 with XIS0 1/8 window no burst, XIS1 1/4 window 0.5 s burst,and XIS3 Psum mode for a exposure of 40 ks. GALACTIC POINT SOURCES 4 A SHIN'YA YAMADA JAP 6 AO6 REVEALING THE NATURE OF FAST TIME VARIABILITY OF CYG X-1 WITH SHOT ANALYSIS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406013010/ Quick Look
78 AXP 4U 0142+614 26.5682 61.7591 25.700455 61.509234 52.151654 46.394786 129.37061357 -0.42523158 40.384 55811.6552314815 2011-09-07 15:43:32 55812.5731134259 2011-09-08 13:45:17 406031010 38.6497 60 38.6497 38.6497 0 38.6825 2 2 0 2 1 0 0 42.1964 42.1964 79.292 0 PROCESSED 57603.1220138889 2016-08-03 02:55:42 56218 2012-10-18 00:00:00 55851.4406828704 2011-10-17 10:34:35 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 060092 We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI. GALACTIC POINT SOURCES 4 A YUJIN NAKAGAWA JAP 6 AO6-TOO A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406031010/ Quick Look
79 HD162020 267.6631 -40.3218 266.786356 -40.308311 268.128314 -16.895672 350.73730077 -6.73005667 259.9987 55829.424212963 2011-09-25 10:10:52 55829.6543865741 2011-09-25 15:42:19 406038030 11.481 10 11.481 11.481 0 11.481 1 1 0 1 1 0 0 8.5402 8.5402 19.8799 0 PROCESSED 57603.2407638889 2016-08-03 05:46:42 56225 2012-10-25 00:00:00 55858.0790162037 2011-10-24 01:53:47 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 061202 Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. GALACTIC POINT SOURCES 4 A IGNAZIO PILLITTERI USA 6 AO6 STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406038030/ Quick Look
80 4 DRA 187.5655 69.216 187.018636 69.492063 136.915856 61.202296 125.72551845 47.79722512 145.5318 55874.1707291667 2011-11-09 04:05:51 55875.0619328704 2011-11-10 01:29:11 406041010 42.258 40 42.258 42.258 0 42.258 2 2 0 2 1 0 0 39.7925 39.7925 76.998 2 PROCESSED 57603.7210532407 2016-08-03 17:18:19 56260 2012-11-29 00:00:00 55890.6961458333 2011-11-25 16:42:27 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 061212 4 Dra is a weakly symbiotic star that exhibited strong variability in ROSAT observations. Our Suzaku Cycle 5 observation confirms it to be an absorbed hard X-ray source, powered by accretion. It is thus a nearby, lower accretion rate analogue of the hard X-ray bright symbiotic stars such as T CrB and CH Cyg. During Suzaku Cycle 6, 4 Dra is near apastron and near the inferior conjunction of the accreting white dwarf: both these should reduce the absorption due to the M giant, while absorption by the accretion flow near the white dwarf should remain roughly comparable. We therefore propose a second Suzaku observation of 4 Dra to constrain the relative contributions of these two X-ray absorbers, and to obtain a high signal-to-noise spectrum of a symbiotic star boundary layer near 1 keV. GALACTIC POINT SOURCES 4 C KOJI MUKAI USA 6 AO6 A SUZAKU OBSERVATION OF 4 DRA NEAR INFERIOR CONJUNCTION XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406041010/ Quick Look
81 4U 1954+31 298.9334 32.0803 298.445315 31.946656 311.138232 51.470698 68.38077131 1.91321277 261.2562 55857.3373263889 2011-10-23 08:05:45 55858.7203009259 2011-10-24 17:17:14 406046010 60.216 60 60.224 60.232 0 60.216 3 2 0 2 1 0 0 57.9008 57.9008 119.4679 0 PROCESSED 57603.6159953704 2016-08-03 14:47:02 56241 2012-11-10 00:00:00 55874.1069328704 2011-11-09 02:33:59 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 061226 We propose the first Suzaku observation of a symbiotic X-ray binary 4U 1954+31. This object has an extraordinarily long spin period, ~5 hour, attributed to the neutron star (NS) rotation, making 4U 1954+31 the slowest-rotating accreting NS binary. It raises a question about its binary evolution, since a slowly rotating NS orbiting an M-type giant is quite unique. As to its large variability, the popular clumpy wind model has not yet become a smoking-gun, and we propose an alternative hypothesis that the NS is a magnetar descendent captured by an M-type giant in their closer encounter. Known X-ray properties of 4U~1954+31 will be revisited in a view of gated accretion onto the strongly magnetized NS. A 60 ks Suzaku observation can examine these scenarios. GALACTIC POINT SOURCES 4 B TERUAKI ENOTO USA 6 AO6 THE SLOWEST ROTATING PULSAR 4U 1954+31 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406046010/ Quick Look
82 GX 17+2 274.0108 -14.0482 273.300467 -14.065956 273.933278 9.337698 16.42401351 1.2676957 264.7715 55853.116099537 2011-10-19 02:47:11 55855.5287037037 2011-10-21 12:41:20 406070010 6.5069 100 6.7572 6.5069 0 6.7572 3 2 0 2 1 0 0 87.3599 87.3599 208.4297 3 PROCESSED 57603.5270023148 2016-08-03 12:38:53 56241 2012-11-10 00:00:00 55873.2944444445 2011-11-08 07:04:00 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 062003 The behaviour of dense matter in neutron stars remains enigmatic. To probe this requires accurate measurements of neutron star radii and masses. We have recently shown that broad relativistic Fe emission lines in neutron star low-mass X-ray binaries can be used to constrain the neutron star radius. These sources also provide another tool, kHz quasi-periodic oscillations (QPOs). Combining a measurement of the velocity of the gas in the inner disk (from the Fe line) and the frequency of the kHz QPOs provides a method to measure the neutron star mass if kHz QPOs originate at the inner disk. We propose 100 ksec observations of GX 349+2 and GX 17+2 to provide a detailed Fe line profile. Simultaneously, we will also observe with RXTE to detect the kHz QPOs, allowing us to test this technique. GALACTIC POINT SOURCES 4 A EDWARD CACKETT EUR 6 AO6 EXPLORING THE IRON LINE - KHZ QPO CONNECTION XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406070010/ Quick Look
83 IGRJ16479-4514 252.0242 -45.1934 251.117904 -45.10536 256.364901 -22.598296 340.16807688 -0.11668459 91.5317 55980.9438194444 2012-02-23 22:39:06 55983.5363541667 2012-02-26 12:52:21 406078010 149.7785 150 149.7865 149.7785 0 149.7865 2 2 0 2 1 0 0 154.7295 154.7295 223.9819 0 PROCESSED 57604.8063888889 2016-08-04 19:21:12 56429 2013-05-17 00:00:00 56062.2788425926 2012-05-15 06:41:32 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 068014 We propose a 100 ks observation of the Supergiant Fast X-ray Transient (SFXT) with the shortest orbital period, the eclipsing IGRJ16479-4514 (3.3 d), with the main aim of probing its X-ray properties along one entire orbital phase with unprecedented sensitivity. The requested net exposure time indeed translates into an observation almost continuously spanning the whole binary system orbit, allowing for the first time an orbital phase resolved investigation of the X-ray emission properties, which will allow us to study the structure of the supergiant companion (its density and ionization state) and to cast light on the outburst mechanism at work in this new class of transients. GALACTIC POINT SOURCES 4 A LARA SIDOLI ARASH BODAGHEE EUS 6 AO6 UNVEILING THE MYSTERY OF THE SUPERGIANT FAST X-RAY TRANSIENT WITH THE SHORTEST ORBITAL PERIOD XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406078010/ Quick Look
84 H1743-322 266.5672 -32.235 265.751321 -32.216345 267.052375 -8.828926 357.25482673 -1.83530791 277.9713 56212.4049884259 2012-10-12 09:43:11 56213.3744560185 2012-10-13 08:59:13 407005030 21.361 40 21.3706 21.3722 0 21.361 3 3 0 3 1 0 0 40.615 40.615 83.736 1 PROCESSED 57607.7385416667 2016-08-07 17:43:30 56598 2013-11-02 00:00:00 56232.473275463 2012-11-01 11:21:31 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A YOSHIHIRO UEDA JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407005030/ Quick Look
85 CYG X-1 299.5875 35.2031 299.117489 35.06664 313.660052 54.251673 71.33506579 3.06957776 88.7802 56390.0953472222 2013-04-08 02:17:18 56391.9585532407 2013-04-09 23:00:19 407015010 4.1499 85 8.503 4.1499 0 66.4751 2 1 0 1 1 0 0 71.7128 71.7128 160.9658 3 PROCESSED 57611.2046875 2016-08-11 04:54:45 56808 2014-05-31 00:00:00 56402.1391087963 2013-04-20 03:20:19 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 070030 We propose to observe Cyg X-1 for 85 ks, utilizing P-sum mode for XIS3. Our aim is to perform shot analysis, which is originally invented by Negoro et al. 1995 with Ginga, and obtain high-quality wide-band spectra for several phases in less than 1 sec; for example, 0.1 sec before the peak, +/- 0.05 sec at the peak, and after the peak. With these spectra, we will quantify changes in five spectral components: hard Comptonization, soft Comptonization, disk emission, Fe-K lines, and reflection. This will be a clue to know long-standing mystery on rapid variability in black holes. GALACTIC POINT SOURCES 4 A SHINYA YAMADA JAP 7 AO7 INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407015010/ Quick Look
86 Z CAM 126.3 73.123 124.909699 73.28505 106.108743 51.709102 141.36861973 32.62424745 91.2043 56239.0368981482 2012-11-08 00:53:08 56239.7800347222 2012-11-08 18:43:15 407016010 35.852 35 35.852 35.852 0 35.852 2 2 0 2 1 0 0 33.8968 33.8968 64.1939 1 PROCESSED 57607.9797337963 2016-08-07 23:30:49 56631 2013-12-05 00:00:00 56264.602349537 2012-12-03 14:27:23 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 070038 Dwarf novae are a subclass of cataclysmic variables, which sometimes show outbursts. In the outbursts, they are considered to emanate disk winds, but observational evidence had been lacking. Recently, our Suzaku observation of Z Cam during a very transition from quiescence to an outburst revealed clear evidence of the disk wind for the first time, and we were able to study characteristics of the disk wind in detail. Z Cam in quiescence, however, has never been observed with high quality instruments. We, therefore, propose an observation of Z Cam in quiescence in order to study entire behavior of the disk wind throughout different phases, combining the existent Suzaku transition phase data and ASCA archival data taken in other phases. GALACTIC POINT SOURCES 4 C KEI SAITOU JAP 7 AO7 COMPREHENSIVE STUDY FOR THE DISK WIND OF THE DWARF NOVA Z CAM THROUGH OUTBURST CYCLES WITH AN OBSERVATION IN QUIESCENCE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407016010/ Quick Look
87 AX J1445.7-5931 221.4519 -59.5275 220.50216 -59.317243 239.705831 -41.083897 316.97780419 0.18867801 281.526 56143.2829513889 2012-08-04 06:47:27 56144.2918865741 2012-08-05 07:00:19 407021010 40.0525 40 41.0682 41.0602 0 40.0525 2 1 0 2 1 0 0 36.8089 36.8089 87.1579 1 PROCESSED 57606.7459722222 2016-08-06 17:54:12 56533 2013-08-29 00:00:00 56167.2116319444 2012-08-28 05:04:45 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 070043 Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. GALACTIC POINT SOURCES 4 A KAZUO MAKISHIMA JAP 7 AO7 ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407021010/ Quick Look
88 IGR J17091-3624 257.2866 -36.4073 256.446112 -36.344023 259.498562 -13.427876 349.52701092 2.20940495 283.8915 56202.8636689815 2012-10-02 20:43:41 56203.7202662037 2012-10-03 17:17:11 407037010 42.0759 120 42.0759 42.0837 0 42.0797 3 3 0 3 1 0 0 40.392 40.392 74.0079 0 PROCESSED 57607.2660069444 2016-08-07 06:23:03 56728 2014-03-12 00:00:00 56226.6701388889 2012-10-26 16:05:00 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 070097 We propose a Suzaku observation of "the second GRS 1915+105" IGR J17091-3624 with a high energy resolution and broadband capability. GRS 1915+105 has been considered to be the unique black hole binary that stays at a high mass accretion rate and shows limit-cycle oscillations, but it was recently discovered that the BHC IGR J17091-3624 has exactly the same X-ray variability patterns as GRS 1915+105. This fact suggests an evidence for common physical mechanism in both system. The Suzaku observation will reveal both similarity and difference with GRS 1915+105 from a point of view of broad-band spectral properties and disk wind, and help us understanding of the accretion flow onto a black hole under a high mass accretion rate. GALACTIC POINT SOURCES 4 B KAZUTAKA YAMAOKA JAP 7 AO7 SUZAKU BROADBAND OBSERVATION OF "THE SECOND GRS 1915+105" IGR J17091-3624 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407037010/ Quick Look
89 PG 1658 +440 254.9348 44.0094 254.55381 44.082621 242.595421 66.02047 69.11167171 38.06633743 330.9998 56115.6740972222 2012-07-07 16:10:42 56116.8301041667 2012-07-08 19:55:21 407040010 51.0329 50 51.0329 51.0329 0 51.0329 1 1 0 1 1 0 0 46.6746 46.6746 99.8718 1 PROCESSED 57606.5897222222 2016-08-06 14:09:12 56508 2013-08-04 00:00:00 56142.1447337963 2012-08-03 03:28:25 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 070112 The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects. GALACTIC POINT SOURCES 4 B ATSUSHI HARAYAMA JAP 7 AO7 SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407040010/ Quick Look
90 BV CEN 202.8234 -54.9803 202.03184 -54.72288 225.050111 -41.512019 308.67903183 7.44609562 120.7167 56329.0246875 2013-02-06 00:35:33 56329.4856018518 2013-02-06 11:39:16 407047010 33.38 30 33.388 33.388 0 33.38 1 1 0 1 1 0 0 30.8692 30.8692 39.8159 0 PROCESSED 57610.5262268518 2016-08-10 12:37:46 56715 2014-02-27 00:00:00 56349.4846990741 2013-02-26 11:37:58 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 071212 The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? GALACTIC POINT SOURCES 4 C KOJI MUKAI USA 7 AO7 DWARF NOVAE WITH EXTREME WHITE DWARF MASSES XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407047010/ Quick Look
91 HERCULES X-1 254.4612 35.329 254.010606 35.404605 245.997214 57.479973 58.13300626 37.51795138 268.1998 56194.4317708333 2012-09-24 10:21:45 56195.0641087963 2012-09-25 01:32:19 407051030 23.5894 20 23.5931 23.5931 0 23.5894 2 2 0 2 1 0 0 23.4769 23.4769 54.634 0 PROCESSED 57607.1945601852 2016-08-07 04:40:10 56689 2014-02-01 00:00:00 56323.5148726852 2013-01-31 12:21:25 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 071224 This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. GALACTIC POINT SOURCES 4 B BRIAN GREFENSTETTE USA 7 AO7 STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407051030/ Quick Look
92 4U1538-522 235.6015 -52.3857 234.665107 -52.226494 246.064673 -31.762519 327.42188954 2.16239803 275.2972 56149.0031134259 2012-08-10 00:04:29 56149.7349537037 2012-08-10 17:38:20 407068010 45.9554 40 45.9554 45.9554 0 45.9554 2 2 0 2 1 0 0 40.05 40.05 63.212 0 PROCESSED 57606.8269444444 2016-08-06 19:50:48 56640 2013-12-14 00:00:00 56272.688900463 2012-12-11 16:32:01 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 071233 Observations of accreting pulsars in High Mass X-ray Binaries (HMXBs) provide us with important information about the physical processes in the stellar wind of the high mass donor star, the coupling between the accreting material and the neutron star's magnetic field, and the physics of the strongly magnetized accretion column above the neutron star. In this proposal we ask for a 40 ks observation of the accreting HMXB 4U1538-522 to conduct the most sensitive study to date of the wide range of characteristics of the broad band (0.1-100 keV) spectrum over a quarter of a binary orbit and with pulse phase. When one considers the ~50% duty cycle of Suzaku observations, the proposed observation will yield coverage of a quarter of the binary orbit. GALACTIC POINT SOURCES 4 A RICHARD ROTHSCHILD USA 7 AO7 THE FIRST SUZAKU OBSERVATION OF 4U1538-522 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407068010/ Quick Look
93 4U 0352+30 58.8427 31.0494 58.059686 30.903757 63.208913 10.461571 163.07655547 -17.13553633 77.7002 56166.360150463 2012-08-27 08:38:37 56170.0980208333 2012-08-31 02:21:09 407088010 153.4893 150 153.4893 153.4893 0 153.4893 2 2 0 2 1 0 0 140.9919 140.9919 322.9236 3 PROCESSED 57607.0637268518 2016-08-07 01:31:46 56582 2013-10-17 00:00:00 56212.7609722222 2012-10-12 18:15:48 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072011 After 40 years of studies, surprisingly little is known about accreting pulsars at low-luminosities, yet these may be the most numerous class of neutron star binaries in the Galaxy. Upcoming large-scale surveys will likely reveal many such objects, but to identify them it is crucial to fully understand their properties. X Per, the archetypal source of this class, at 1 kpc from Earth is ideal target for detailed studies. In spite of that X Per is still puzzling. With the proposed program we aim to study X Per in detail, constrain its X-ray spectrum also as a function of the spin phase. Our study will be key to characterize the properties of low-luminosity X-ray pulsars population and will help to identify it in upcoming surveys. GALACTIC POINT SOURCES 4 B VICTOR DOROSHENKO EUR 7 AO7 CRACKING THE X PER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407088010/ Quick Look
94 J1522-5734 230.5286 -57.5816 229.552952 -57.402737 244.521376 -37.577548 322.05619938 -0.4156844 274.4971 56154.6486342593 2012-08-15 15:34:02 56155.0078356482 2012-08-16 00:11:17 407094010 30.0295 25 30.0455 30.0295 0 30.0455 1 1 0 1 1 0 0 23.6862 23.6862 31.0239 0 PROCESSED 57606.8538194444 2016-08-06 20:29:30 56638 2013-12-12 00:00:00 56272.6647222222 2012-12-11 15:57:12 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 072019 The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. GALACTIC POINT SOURCES 4 A MARTINO MARELLI EUR 7 AO7 SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407094010/ Quick Look
95 4U 0142+61 26.5838 61.7628 25.715895 61.512967 52.16359 46.394147 129.37704782 -0.4200572 82.997 56504.4205902778 2013-07-31 10:05:39 56506.6252430556 2013-08-02 15:00:21 408011010 101.1678 100 101.1678 101.1828 0 101.1828 2 2 0 2 1 0 0 102.4739 102.4739 190.4637 1 PROCESSED 57612.1558680556 2016-08-12 03:44:27 56953 2014-10-23 00:00:00 56587.5059606482 2013-10-22 12:08:35 3.0.22.44 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 080035 A toroidal magnetic field is thought to be formed in neutron star interior after core-collapse supernovae and become an energy source with recently observed X-ray outbursts from magnetars. Since the toroidal field is hidden in the stellar interior, it was thought to be undetectable via the well-known p-pdot method and the cyclotron resonance scattering features. However, a magnetic stress of the magnetar toroidal field is strong enough to distort the stellar shape and produce a free precession in its X-ray pulse timing if the emission pattern deviates from its axis of symmetry. From our analyses of magnetar 4U 0142+61, we found an evidence on the free precession in the hard X-ray component. To confirm and establish this evidence, we propose an additional 100 ks observation of 4U 0142+61. GALACTIC POINT SOURCES 4 A TERUAKI ENOTO JAP 8 AO8 TOROIDAL FIELD INSIDE MAGNETARS OBSERVED WITH SUZAKU TIMING ANALYSES OF ITS FREE PRECESSION XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408011010/ Quick Look
96 SGR 0501+4516 75.2774 45.2864 74.365802 45.213531 78.849797 22.414701 161.53821228 1.95483036 87.7054 56535.9761574074 2013-08-31 23:25:40 56536.8752662037 2013-09-01 21:00:23 408013010 36.1244 40 36.1244 41.2611 0 41.2452 2 2 0 1 1 0 0 35.7177 35.7177 77.6719 1 PROCESSED 57612.459375 2016-08-12 11:01:30 56974 2014-11-13 00:00:00 56608.6586342593 2013-11-12 15:48:26 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 080040 Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources. GALACTIC POINT SOURCES 4 B TERUAKI ENOTO JAP 8 AO8 ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408013010/ Quick Look
97 SAGITTARIUS A* 266.4146 -29.0065 265.619896 -28.987158 266.840205 -5.604694 359.94434823 -0.0438121 107.0001 56728.6474537037 2014-03-12 15:32:20 56729.1147569445 2014-03-13 02:45:15 408017060 21.1387 20 21.1427 21.1387 0 21.1595 2 2 0 3 1 0 0 20.4844 20.4844 40.368 0 PROCESSED 57614.0078240741 2016-08-14 00:11:16 57113 2015-04-01 00:00:00 56747.6540972222 2014-03-31 15:41:54 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 080074 With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. GALACTIC POINT SOURCES 4 A YOSHITOMO MAEDA JAP 8 AO8 SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017060/ Quick Look
98 SWIFT J2319.4+2619 349.8819 26.2473 349.265885 25.973522 2.029717 27.934963 98.48369948 -32.22425134 253.9963 56633.8796875 2013-12-07 21:06:45 56634.8786111111 2013-12-08 21:05:12 408030010 41.2758 40 41.2758 41.2758 0 41.2758 1 1 0 1 1 0 0 38.149 38.149 86.2879 2 PROCESSED 57613.5369328704 2016-08-13 12:53:11 57039 2015-01-17 00:00:00 56672.6300578704 2014-01-15 15:07:17 3.0.22.44 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 081213 Polars are a subclass of magnetic cataclysmic variables in which a strongly magnetic white dwarf accretes matter from a late-type, Roche-lobe filling mass donor. They are usually soft X-ray bright and hard X-ray dim, due to either buried shocks or strong cyclotron cooling, depending on system parameters. However, a small subset of polars have been detected as bright hard X-ray sources in INTEGRAL and Swift BAT surveys. As a part of an effort to understand the hard-to-soft X-ray luminosity ratios of polars in general, and specifically to understand what combination of parameters make some polars hard X-ray bright, we propose Suzaku observations of two poorly studied BAT polars, Swift J2319.4+2619 and IW Eri, supported by ground-based observations including optical polarimetry. GALACTIC POINT SOURCES 4 C KOJI MUKAI USA 8 AO8 THE HARD X-RAY BRIGHT POLARS SWIFT J2319.4+2619 AND IW ERI XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408030010/ Quick Look
99 SERPENS X-1 279.9874 5.0445 279.370748 4.997683 281.283069 28.094693 36.12473115 4.84817413 93.4997 56729.1215277778 2014-03-13 02:55:00 56731.6459606482 2014-03-15 15:30:11 408033020 1.2154 120 6.5666 24.0772 0 1.2154 2 2 0 2 1 0 0 82.3578 82.3578 218.0879 4 PROCESSED 57614.078912037 2016-08-14 01:53:38 57198 2015-06-25 00:00:00 56747.822037037 2014-03-31 19:43:44 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 081222 Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs. GALACTIC POINT SOURCES 4 B EDWARD CACKETT USA 8 AO8 THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408033020/ Quick Look
100 SERPENS X-1 279.9877 5.0424 279.371038 4.995582 281.28322 28.092576 36.12298663 4.84695852 81.3009 56757.3507060185 2014-04-10 08:25:01 56757.8959259259 2014-04-10 21:30:08 408033030 0.388 25 1.8071 6.4595 0 0.388 3 3 0 3 1 0 0 23.0266 23.0266 47.0979 0 PROCESSED 57614.2331481482 2016-08-14 05:35:44 57198 2015-06-25 00:00:00 56821.7352430556 2014-06-13 17:38:45 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 081222 Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs. GALACTIC POINT SOURCES 4 B EDWARD CACKETT USA 8 AO8 THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408033030/ Quick Look
101 X 1630-472 248.5012 -47.3939 247.580186 -47.289758 254.085797 -25.132076 336.90807869 0.25236055 88.6321 57077.0625578704 2015-02-24 01:30:05 57078.1140277778 2015-02-25 02:44:12 409007020 5.5296 40 5.547 5.5659 0 5.5296 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57617.6879282407 2016-08-17 16:30:37 57454 2016-03-07 00:00:00 57087.4605208333 2015-03-06 11:03:09 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 090015 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A YOSHIHIRO UEDA JAP 9 AO9-TOO MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409007020/ Quick Look
102 H1743-322 266.2607 -32.2285 265.444935 -32.208359 266.789922 -8.828952 357.12541364 -1.6105206 285.4288 56932.6365625 2014-10-02 15:16:39 56933.284837963 2014-10-03 06:50:10 409008010 15.0094 40 15.6012 15.6169 0 15.0094 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57616.6096527778 2016-08-16 14:37:54 57345 2015-11-19 00:00:00 56979.4022569444 2014-11-18 09:39:15 3.0.22.44 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 090015 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A YOSHIHIRO UEDA JAP 9 AO9-TOO MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409008010/ Quick Look
103 H1743-322 266.5672 -32.2343 265.751326 -32.215645 267.052358 -8.828226 357.25542532 -1.83494451 273.3773 56939.7339236111 2014-10-09 17:36:51 56940.5245138889 2014-10-10 12:35:18 409008020 19.0006 40 19.0006 19.0145 0 19.0115 3 3 0 3 0 0 0 0 0 0 0 PROCESSED 57616.6317824074 2016-08-16 15:09:46 57345 2015-11-19 00:00:00 56979.407974537 2014-11-18 09:47:29 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 090015 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A YOSHIHIRO UEDA JAP 9 AO9-TOO MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409008020/ Quick Look
104 SAGITTARIUS A* 266.4193 -29.0102 265.624572 -28.990881 266.844426 -5.60829 359.94333122 -0.04924818 267.3027 56929.1441550926 2014-09-29 03:27:35 56929.6668402778 2014-09-29 16:00:15 409011010 20.2183 20 20.2183 20.3303 0 20.3543 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57616.5861226852 2016-08-16 14:04:01 56748 2014-04-01 00:00:00 56979.4039814815 2014-11-18 09:41:44 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 090048 With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window. GALACTIC POINT SOURCES 4 A YOSHITOMO MAEDA JAP 9 AO9 SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011010/ Quick Look
105 SAGITTARIUS A* 266.4217 -29.0078 265.626986 -28.988492 266.846474 -5.605838 359.94647323 -0.04978962 278.8011 56938.0879861111 2014-10-08 02:06:42 56938.4619097222 2014-10-08 11:05:09 409011020 17.2605 20 17.2605 17.2605 0 17.2605 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57616.6209606482 2016-08-16 14:54:11 56748 2014-04-01 00:00:00 56979.4091087963 2014-11-18 09:49:07 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 090048 With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window. GALACTIC POINT SOURCES 4 A YOSHITOMO MAEDA JAP 9 AO9 SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011020/ Quick Look
106 1RXSJ182853.8-241746 277.2212 -24.2932 276.455559 -24.326354 276.570172 -1.017121 8.76671438 -6.19414371 87.3419 57120.5005092593 2015-04-08 12:00:44 57120.8217476852 2015-04-08 19:43:19 409013010 9.7072 12 9.7072 11.8422 0 11.8502 3 2 0 2 0 0 0 0 0 0 0 PROCESSED 57617.9447453704 2016-08-17 22:40:26 57496 2016-04-18 00:00:00 57129.4074189815 2015-04-17 09:46:41 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 090051 We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. GALACTIC POINT SOURCES