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 | LOW_LATITUDE_86-21 | 332.3169 | 30.2173 | 331.751825 | 29.971433 | 347.602182 | 38.425077 | 86.0039952 | -20.78963339 | 82.7457 | 54229.0809259259 | 2007-05-09 01:56:32 | 54230.9966898148 | 2007-05-10 23:55:14 | 502047010 | 81.5486 | 80 | 81.5486 | 81.5486 | 0 | 81.5486 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72.2931 | 72.2931 | 165.5099 | 2 | PROCESSED | 57538.6557986111 | 2016-05-30 15:44:21 | 54744 | 2008-10-05 00:00:00 | 54244.7948032407 | 2007-05-24 19:04:31 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020061 | High galactic-latitude Suzaku observations of soft X-ray diffuse emission so far made show general tendency that the OVII emission line becomes stronger with decreasing abs(b). This suggests that the major part of the emission is originating from the halo of our galaxy. However, we cannot rule out the possibility that the data is contaminated by solar wind charge exchange emission from the entire heliosphere. In oder to confirm the abs(b) dependency and to constrain the spatial distribution of the halo emission, we propose to observe diffuse radiation at a low galactic latitude of abs(b) ~ 20 deg, where the galactic absorption still does not affect the line intensity significantly. | GALACTIC DIFFUSE EMISSION | 5 | B | TOMOTAKA YOSHINO | JAP | 2 | AO2 | SOFT X-RAY DIFFUSE EMISSION AT A LOW GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502047010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '502047010'
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