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 | VICINITY OF LMC X-3 | 83.4844 | -63.8863 | 83.408578 | -63.918105 | 41.435206 | -86.187449 | 273.3865557 | -32.64248934 | 284.6189 | 53811.6008333333 | 2006-03-17 14:25:12 | 53813.9168055556 | 2006-03-19 22:00:12 | 500031010 | 82.0185 | 80 | 82.0265 | 82.0185 | 82.0265 | 82.0265 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 74.6148 | 74.6148 | 200.0639 | 2 | PROCESSED | 57533.2849537037 | 2016-05-25 06:50:20 | 54247 | 2007-05-27 00:00:00 | 54056.4806828704 | 2006-11-17 11:32:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000043 | We propose to observe the vicnity of LMC X-3 for 80 ks. We expectt to determine the OVII and OVIII emission line intensities within 20% errors. Combining these results with the OVII and OVIII absorption lines observed in the energy spectra of LMC X-3 with Chandra LETG-HRC, we can determine the geometrocal extent od the hot gas along the line-of-sight direction. This will answer the long-unanswered question; from where the high lattitude OVII/OVIII emissions come ? | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | JAP | 0 | SWG | VICINITY OF LMC X-3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500031010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '500031010'
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