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 | HESS J1745-303 2 | 266.4705 | -30.0867 | 265.668866 | -30.067612 | 266.916061 | -6.683329 | 359.0474588 | -0.64781783 | 70.5003 | 54531.5601388889 | 2008-03-06 13:26:36 | 54533.6669444444 | 2008-03-08 16:00:24 | 502017010 | 72.5443 | 67 | 72.5523 | 72.5523 | 0 | 72.5443 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63.9723 | 63.9723 | 182.0149 | 2 | PROCESSED | 57541.8457291667 | 2016-06-02 20:17:51 | 54919 | 2009-03-29 00:00:00 | 54550.4057986111 | 2008-03-25 09:44:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020023 | A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | B | RYO YAMAZAKI | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502017010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '502017010'
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