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 | SNR G304.6+0.1 | 196.4463 | -62.6951 | 195.657347 | -62.427468 | 227.041423 | -49.777353 | 304.57643925 | 0.13082789 | 321.0575 | 55442.9126736111 | 2010-09-03 21:54:15 | 55445.5356828704 | 2010-09-06 12:51:23 | 505074010 | 99.5817 | 100 | 99.6217 | 99.5817 | 0 | 99.6297 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90.5653 | 90.5653 | 226.5319 | 1 | PROCESSED | 57553.3505555556 | 2016-06-14 08:24:48 | 55827 | 2011-09-23 00:00:00 | 55461.4231712963 | 2010-09-22 10:09:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051306 | Galactic supernova remnants are believed to be the primary source of cosmic rays below 10^15.5 eV even though the exact acceleration mechanism remains unknown. This uncertainty results from the lack of remnants with synchrotron X-ray and GeV emission, needed to distinguish accelerated electrons from protons using broadband spectral modeling. An analysis of recent XMM and Fermi data suggests SNR G304.6+0.1 is just the third remnant with both, but the observed hard X-ray excess is also consistent with bremsstrahlung emission. We request a deep Suzaku observation of this source to determine the nature of its hard X-ray emission - critical for identifying the underlying acceleration mechanism. | GALACTIC DIFFUSE EMISSION | 5 | B | JOSEPH GELFAND | USA | 5 | AO5 | THE ORIGIN OF THE HARD X-RAY AND GEV GAMMA-RAY EMISSION OF SNR G304.6+0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505074010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '505074010'
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