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 | HESSJ1857-A | 284.2126 | 2.7519 | 283.584668 | 2.685017 | 285.744612 | 25.418977 | 35.99783049 | 0.0515802 | 269.8116 | 55822.9197800926 | 2011-09-18 22:04:29 | 55823.984212963 | 2011-09-19 23:37:16 | 506019010 | 40.9249 | 40 | 40.9249 | 40.9249 | 0 | 40.9249 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.8469 | 35.8469 | 91.9279 | 1 | PROCESSED | 57603.2046180556 | 2016-08-03 04:54:39 | 56233 | 2012-11-02 00:00:00 | 55865.2326157407 | 2011-10-31 05:34:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060061 | Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not. | GALACTIC DIFFUSE EMISSION | 5 | B | HIRONORI MATSUMOTO | JAP | 6 | AO6 | ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506019010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '506019010'
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