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 | GC_G0.9+0.1 | 266.9332 | -28.1474 | 266.1438 | -28.130586 | 267.277369 | -4.735296 | 0.91503767 | 0.01290063 | 105.8953 | 54536.2637152778 | 2008-03-11 06:19:45 | 54540.229375 | 2008-03-15 05:30:18 | 502051010 | 138.7614 | 133 | 138.7614 | 138.7614 | 0 | 138.7614 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 122.2214 | 122.2214 | 342.5768 | 1 | PROCESSED | 57541.9299305556 | 2016-06-02 22:19:06 | 54919 | 2009-03-29 00:00:00 | 54550.6988078704 | 2008-03-25 16:46:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020071 | The Suzaku PV observations found that the diffuse X-rays (6.7 and 6.9 keV-lines) from the GC region can well be explained by a thermal emission from hot plasma (6-7 keV). The most plausible energy injection source is multiple SNe. The huge thermal energy (10^54 ergs) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm this scenario, we propose to observe the shell of G0.9+0.1 and the connecting region of Sgr B and D. The first objective is to detect a thermal emission from the shell of G0.9+0.1 and the second is to discover new SNRs. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 2 | AO2 | SNR G0.9+0.1 AND THE CONNECTING REGION OF SGR B AND D | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502051010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '502051010'
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