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 | W51SW | 290.8908 | 14.1062 | 290.315286 | 14.008227 | 295.206632 | 35.736826 | 49.1149541 | -0.54215584 | 104.3698 | 55285.3081944444 | 2010-03-30 07:23:48 | 55286.3752314815 | 2010-03-31 09:00:20 | 504067010 | 43.7287 | 40 | 43.7287 | 43.7287 | 0 | 43.7287 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.8137 | 9.8137 | 92.1799 | 0 | PROCESSED | 57551.0856597222 | 2016-06-12 02:03:21 | 55671 | 2011-04-20 00:00:00 | 55302.2468055556 | 2010-04-16 05:55:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040129 | We propose to observe the supernova remnant (SNR) W51C with Suzaku XIS. The thermal energy of plasma in W51C, ~3x10^51ergs, is much larger than typical kinetic energy of supernova and can give a large amount of energy to cosmic-ray acceleration. The SNR interactes with the giant molecler cloud and is expected to emit gamma-rays from cosmic-ray interaction. We search for non-thermal X-ray diffuse emission from electron bremsstrahlung or synchrotron emission of secondary electrons produced by decaying charged pions created by p-p interaction. | GALACTIC DIFFUSE EMISSION | 5 | C | HIDEAKI KATAGIRI | JAP | 4 | AO4 | ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504067010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '504067010'
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