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 V2301 OPH 270.1519 8.1612 269.551065 8.161911 270.165981 31.601449 34.53664844 14.98247082 262.0703 56573.9878356482 2013-10-08 23:42:29 56576.0002893518 2013-10-11 00:00:25 408024010 40.1356 150 40.1356 40.1356 0 40.1356 2 2 0 2 1 0 0 65.6843 65.6843 173.8587 1 PROCESSED 57612.9068981482 2016-08-12 21:45:56 57184 2015-06-11 00:00:00 56596.5744907407 2013-10-31 13:47:16 3.0.22.44 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 080107 It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion. GALACTIC POINT SOURCES 4 A TAKAYUKI HAYASHI JAP 8 AO8 MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408024010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '408024010'

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