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 S2 128.0787 -47.1859 127.674645 -47.014943 154.605433 -62.350481 264.85904608 -4.40317226 122.1879 56989.4162847222 2014-11-28 09:59:27 56989.8404976852 2014-11-28 20:10:19 509018010 17.4774 15 17.4774 17.4774 0 17.4774 1 1 0 1 0 0 0 0 0 0 0 PROCESSED 57617.4063773148 2016-08-17 09:45:11 57368 2015-12-12 00:00:00 57002.436087963 2014-12-11 10:27:58 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/ver3.0/509018010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '509018010'

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