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 | VELA PWN S1 | 128.1818 | -46.8811 | 127.77491 | -46.709753 | 154.389152 | -62.054406 | 264.65396784 | -4.16648977 | 122.1894 | 56988.5541087963 | 2014-11-27 13:17:55 | 56988.8905324074 | 2014-11-27 21:22:22 | 509017010 | 15.4638 | 15 | 15.4638 | 15.4878 | 0 | 15.7838 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8238194444 | 2016-08-16 19:46:18 | 57368 | 2015-12-12 00:00:00 | 57002.4344328704 | 2014-12-11 10:25:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, 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. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509017010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '509017010'
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