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 SS CYG 325.6842 43.5739 325.1931 43.344666 350.456739 52.648094 90.55430501 -7.12254626 256.8767 53692.6066203704 2005-11-18 14:33:32 53693.8646759259 2005-11-19 20:45:08 400007010 56.043 60 56.059 56.179 56.043 56.059 2 2 2 2 1 0 0 54.3572 54.3572 108.6658 2 PROCESSED 57528.0435763889 2016-05-20 01:02:45 54247 2007-05-27 00:00:00 54037.9128472222 2006-10-29 21:54:30 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 001044 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-TOO SS CYG OBSERVATION IN OUTBURST XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400007010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '400007010'

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