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 IGR J15094-6649 227.3484 -66.8278 226.235673 -66.63712 247.091848 -46.74399 315.91945149 -7.50109233 90.4626 55588.7031365741 2011-01-27 16:52:31 55589.5557638889 2011-01-28 13:20:18 405007010 49.4612 50 49.4832 49.4752 0 49.4612 2 2 0 2 1 0 0 48.0185 48.0185 73.6599 0 PROCESSED 57600.7830092593 2016-07-31 18:47:32 55990 2012-03-04 00:00:00 55621.2282291667 2011-03-01 05:28:39 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 050025 The all-sky survey in hard X-rays with INTEGRAL has been finding new magnetic Cataclysmic Variables. Among them, we propose Suzaku observations of five Intermediate Polars (IPs) which have no detailed follow-up spectroscopy in the hard X-ray band up to now. The wide-band energy coverage of Suzaku, therefore, is definitely useful to extract physical information from their spectra since, generally, the vFv spectrum of an IP peaks at E=20-50 keV and strong intrinsic absorption (nH=1E22-23 cm-2). By fitting the spectrum with our numerical model, we estimate a plasma temperature and an Fe abundance, and furthermore, a white dwarf mass which is one of the most basic and important parameter of a binary system. GALACTIC POINT SOURCES 4 C TAKAYUKI YUASA JAP 5 AO5 ESTIMATE MASSES OF NEWLY-FOUND MAGNETIC WHITE DWARFS BASED ON HARD X-RAY CONTINUUM AND FE EMISSION LINES XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405007010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '405007010'

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