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 | KEPLER | 262.6698 | -21.4886 | 261.920525 | -21.451271 | 263.169114 | 1.778808 | 4.51918955 | 6.82146946 | 98.2145 | 54514.1665393518 | 2008-02-18 03:59:49 | 54516.9793287037 | 2008-02-20 23:30:14 | 502078010 | 116.9636 | 100 | 116.9636 | 116.9636 | 0 | 116.9636 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98.9551 | 98.9551 | 242.9956 | 3 | PROCESSED | 57541.7751388889 | 2016-06-02 18:36:12 | 54894 | 2009-03-04 00:00:00 | 54525.6176851852 | 2008-02-29 14:49:28 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 023074 | We propose to observe the Kepler's SNR in which evidence of particle acceleration will be found. Aim of the observation is to determine power-law contribution in the hard-tail spectrum above 10 keV with HXD-PIN. If we also find the Fe-Kb and Ni-K emission lines with XIS which have not observed in any previous missions, temperature and nt parameter of a NEI model will be fixed. The determination will help to distinguish the power-law component from the thermal one. We also memtioned that the amount of Fe and Ni will be a good estimator to determine the type of Kepler's SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | TORU TAMAGAWA | Sangwook Park | JUS | 2 | AO2 | SEARCH FOR EVIDENCE OF COSMIC-RAY ACCELERATION IN THE KEPLER'S SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502078010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '502078010'
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