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 HESS J1745-303 1 266.2249 -30.1096 265.423171 -30.089321 266.702778 -6.71164 358.91712668 -0.478438 70.5005 54527.7555555556 2008-03-02 18:08:00 54529.7363310185 2008-03-04 17:40:19 502016010 70.5291 67 70.5371 70.5291 0 70.5451 2 2 0 2 1 0 0 61.7932 61.7932 171.0959 3 PROCESSED 57541.8000810185 2016-06-02 19:12:07 54908 2009-03-18 00:00:00 54539.3190509259 2008-03-14 07:39:26 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/ver3.0/502016010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '502016010'

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