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
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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