DARTS/Astro Query System - SQL Search -
All the tables available for SQL Search and information on each table are listed in the Available Data page. Please see the User Guide for the usage of "SQL Search".
total 1
No. |
object_name
|
center_ra
|
center_dec
|
center_ra_b1950
|
center_dec_b1950
|
center_ecliptic_lon
|
center_ecliptic_lat
|
center_galactic_lon
|
center_galactic_lat
|
roll_angle
|
observation_start_time_mjd
|
observation_start_time
|
observation_end_time_mjd
|
observation_end_time
|
observation_id
|
exposure
|
awarded_exposure
|
xis0_exposure
|
xis1_exposure
|
xis2_exposure
|
xis3_exposure
|
xis0_observation_mode
|
xis1_observation_mode
|
xis2_observation_mode
|
xis3_observation_mode
|
hxd_observation_mode
|
hxd_coarse_clock_rate_exposure
|
hxd_first_clock_rate_exposure
|
hxd_normal_clock_rate_exposure
|
hxd_all_clock_rate_exposure
|
hxd_wam_exposure
|
quantity_of_hxd_burst
|
processing_status
|
processing_date_mjd
|
processing_date
|
public_date_mjd
|
public_date
|
distribution_date_mjd
|
distribution_date
|
processing_version
|
processing_count
|
processing_software
|
proposal_id
|
proposal_abstract
|
proposal_category
|
proposal_category_code
|
proposal_priority
|
pi_name
|
co_pi_name
|
proposal_affiliated_country
|
proposal_cycle
|
observation_type
|
proposal_title
|
main_instrument
|
has_xis_injection
|
data_access_url
|
ql_access_url
|
ql_image_url
|
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1 | U GEM IN QUIECSECNCE | 118.777 | 21.9977 | 118.037172 | 22.130129 | 116.517698 | 1.166962 | 199.22882002 | 23.39765052 | 280.879 | 56041.5636921296 | 2012-04-24 13:31:43 | 56044.5765856482 | 2012-04-27 13:50:17 | 407034010 | 119.1136 | 120 | 119.1136 | 119.1136 | 0 | 119.1136 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 102.8354 | 102.8354 | 260.306 | 1 | PROCESSED | 57605.3496064815 | 2016-08-05 08:23:26 | 56434 | 2013-05-22 00:00:00 | 56068.6228356482 | 2012-05-21 14:56:53 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070065 | It has been believed that the optically thin boundary layer in dwarf novae (DNe) turns into optically thick state in outburst, and, as a result, hard optically thin X-ray emission becomes weaker than in quiescence. This theory was verified in multi-waveband observations of SS Cyg. The DN U Gem, however, does not follow this scenario, and the hard X-ray intensity increases in outburst as well as soft X-ray emission. We propose ToO observations of U Gem both in quiescence and in outburst in order to understand behavior of DNe in X-rays in general, by means of detailed spectroscopy of the soft disk blackbody component, the hard component reflected off the white dwarf, and a 6.4 keV iron line. This study eventually enables us to understand the origin of the Galactic Ridge X-ray Emission. | GALACTIC POINT SOURCES | 4 | B | TAKAYUKI HAYASHI | JAP | 7 | AO7-TOO | OBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407034010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '407034010'
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