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 EP DRA 286.7359 69.1573 286.793684 69.076999 30.014466 83.210835 100.08892772 23.87463538 44.5637 57164.4409953704 2015-05-22 10:35:02 57166.2856365741 2015-05-24 06:51:19 410006010 80.2346 80 80.2346 80.2426 0 80.2426 2 2 0 2 1 0 0 67.9585 67.9585 155.5819 1 PROCESSED 57618.7517939815 2016-08-18 18:02:35 57558 2016-06-19 00:00:00 57176.3159027778 2015-06-03 07:34:54 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 100018 It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar mass (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 mass and approach 3.3 solar mass. We will get observational relations between WD mass and radius for proposed targets with Suzaku. With WD masses dynamically measured, we can estimate the WD radii without any theoretical mass-radius relation. We will be able to, for the first time, observationally investigate the influence of magnetic field on EOS in WDs and the WD mass-radius relation by the estimating WD radii and masses. GALACTIC POINT SOURCES 4 A TAKAYUKI HAYASHI JAP 10 AO10 CONSTRAINT ON MASS-RADIUS RELATION OF HIGHLY MAGNETIZED WHITE DWARFS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410006010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '410006010'

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