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 | GK PER | 52.8052 | 43.8974 | 51.953057 | 43.727495 | 61.505862 | 24.068527 | 150.96310366 | -10.10758836 | 250.0842 | 57086.777037037 | 2015-03-05 18:38:56 | 57090.7709606482 | 2015-03-09 18:30:11 | 409018020 | 182.886 | 140 | 0 | 0 | 0 | 182.886 | 0 | 0 | 0 | 2 | 1 | 0 | 0 | 134.9166 | 134.9166 | 344.9376 | 0 | PROCESSED | 57617.786712963 | 2016-08-17 18:52:52 | 57468 | 2016-03-21 00:00:00 | 57101.0913657407 | 2015-03-20 02:11:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090055 | A 140-ks observation of the magnetic cataclysmic variable GK Per is proposed. By fitting Suzaku broadband spectra using our multitemperature spectral model of the accretion column, we estimate a white dwarf mass with statistical fitting errors smaller than 5%. The estimated mass will be compared with one obtained from the optical lightcurve fitting method developed and applied by Hachisu and Kato in a series of papers. GK Per is the only known magnetic cataclysmic variable which underwent classical nova explosion (in 1901), and both the mass estimation methods can be applied. Cross-validated WD mass estimation methods will be of importance in studying massive white dwarfs in accretion systems, in relation with the progenitor of type Ia supernovae. | GALACTIC POINT SOURCES | 4 | A | TAKAYUKI YUASA | JAP | 9 | AO9 | CROSS VALIDATION OF WHITE DWARF MASS ESTIMATION METHODS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409018020/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '409018020'
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