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 | BV CEN | 202.8234 | -54.9803 | 202.03184 | -54.72288 | 225.050111 | -41.512019 | 308.67903183 | 7.44609562 | 120.7167 | 56329.0246875 | 2013-02-06 00:35:33 | 56329.4856018518 | 2013-02-06 11:39:16 | 407047010 | 33.38 | 30 | 33.388 | 33.388 | 0 | 33.38 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 30.8692 | 30.8692 | 39.8159 | 0 | PROCESSED | 57610.5262268518 | 2016-08-10 12:37:46 | 56715 | 2014-02-27 00:00:00 | 56349.4846990741 | 2013-02-26 11:37:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407047010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '407047010'
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