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 | 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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