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
1 VELA PWN W3 126.9052 -45.2087 126.488861 -45.042306 150.998783 -61.06652 262.77480933 -3.90558145 95.0008 56590.9784606482 2013-10-25 23:28:59 56591.4343055556 2013-10-26 10:25:24 508044010 13.871 15 13.871 13.871 0 13.871 2 2 0 2 1 0 0 11.3448 11.3448 39.3799 1 PROCESSED 57613.1197106482 2016-08-13 02:52:23 57009 2014-12-18 00:00:00 56643.6595949074 2013-12-17 15:49:49 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 080090 We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. GALACTIC DIFFUSE EMISSION 5 B KOJI MORI JAP 8 AO8 SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508044010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '508044010'

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