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 V773TAU 63.5571 28.1952 62.783682 28.069565 66.716115 6.867305 168.22500409 -16.34364304 260.6557 55610.1581712963 2011-02-18 03:47:46 55611.9815277778 2011-02-19 23:33:24 405011010 82.2463 80 82.2543 82.2463 0 82.2543 2 2 0 2 1 0 0 72.8287 72.8287 157.5258 2 PROCESSED 57601.0256134259 2016-08-01 00:36:53 55990 2012-03-04 00:00:00 55621.2978703704 2011-03-01 07:08:56 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 050033 We propose a Suzaku observation of the pre-main sequence binary system V773 Tau with the high sensitivity of HXD. The empirical Lx-Lr relation (Benz-G"udel relation) and radio flux variation predict that this source can have a flare with a peak luminosity Lx=10^34 ergs s-1, seven orders of magnitude larger than that of the Sun, when it is just before the periastron passage. We will observe this target simultaneously with radio band using VLBI network. Our goal is (1) to test whether the gigantic flare is still on the empirical relation (2) to detect inpulsive non-thermal emission at the most powerful stellar flare (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band. GALACTIC POINT SOURCES 4 B YOHKO TSUBOI JAP 5 AO5 NON-THERMAL EMISSION AT THE MOST POWERFUL STELLAR FLARE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405011010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '405011010'

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