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 | M17 | 275.2076 | -16.1829 | 274.486266 | -16.206429 | 275.030512 | 7.16685 | 15.0906551 | -0.7606192 | 110.1996 | 53805.8263425926 | 2006-03-11 19:49:56 | 53808.5349421296 | 2006-03-14 12:50:19 | 501003010 | 102.7021 | 100 | 102.7101 | 102.7101 | 102.7021 | 102.7101 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 92.5661 | 92.5661 | 233.9678 | 4 | PROCESSED | 57533.2492939815 | 2016-05-25 05:58:59 | 54394 | 2007-10-21 00:00:00 | 53905.822662037 | 2006-06-19 19:44:38 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010066 | Recent Chandra observations discovered that HII regions possess a few MK extended plasma, but the origin of the emission is still unknown. We propose to observe M17, which has the most spectacular sample of such emission. A superb soft-band response of XIS will enable us to measure the strengths of O and N emission lines, giving us strong arguments to elucidate the cause of the emission. A 300 ks Chandra observation is planned this year in addition to the existing 40 ks data, which will help us to discriminate the point source contribution. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAHIRO TSUJIMOTO | JAP | 1 | AO1 | XIS INVESTIGATION FOR THE ORIGIN OF DIFFUSE X-RAY EMISSION IN GALACTIC H II REGIONS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501003010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '501003010'
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