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 | PKS2155-304 | 329.7191 | -30.2247 | 328.99529 | -30.464273 | 321.189186 | -16.770975 | 17.73226544 | -52.24760927 | 254.1358 | 53704.7749884259 | 2005-11-30 18:35:59 | 53706.3613888889 | 2005-12-02 08:40:24 | 700012010 | 63.9114 | 80 | 63.9194 | 63.9114 | 63.9194 | 63.9166 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 58.0114 | 58.0114 | 137.0498 | 3 | PROCESSED | 57532.3797685185 | 2016-05-24 09:06:52 | 54247 | 2007-05-27 00:00:00 | 54038.8920138889 | 2006-10-30 21:24:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001100 | Jets in blazars are believed to be a powerful site of particle acceleration. TeV emitting blazars are very important, because we can study very end of electron distribution near the maximum energy by using X-ray spectrum, because X-ray emission is believed to be due to synchrotron emission from the higher energy electron. Comparison of spectral index between X-ray and TeV gives us a crucial information on these source, because this is very sensitive to the particle injection and rapid cooling. In order to maximize the capability of sensitive hard X-ray observations of Suzaku, we propose reserved TOO observations for the next six months of PV phase from the TeV emitting blazars established by HESS, selected from five candidates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 0 | SWG-TOO | RESERVED TOO OBSERVATIONS OF SELECTED TEV-BRIGHT BLAZARS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700012010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '700012010'
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