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 | T PYXIDIS | 136.1704 | -32.3688 | 135.652133 | -32.168809 | 152.023797 | -46.371088 | 257.19727302 | 9.71237496 | 121.9943 | 56266.272662037 | 2012-12-05 06:32:38 | 56268.8695486111 | 2012-12-07 20:52:09 | 407048010 | 86.676 | 100 | 86.676 | 86.676 | 0 | 86.676 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73.6118 | 73.6118 | 224.3579 | 4 | PROCESSED | 57608.249525463 | 2016-08-08 05:59:19 | 56660 | 2014-01-03 00:00:00 | 56291.8230787037 | 2012-12-30 19:45:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071213 | We propose a 100 ks observation of the classical nova remnant in the accreting binary system T Pyxidis using Suzaku. T Pyxidis is a system which causes a cycle of classical nova outbursts in a decade time scale. Shocks might occur in the ejecta, and X-rays were detected from its spatially-resolved expanding shell like a miniature supernova remnant. The immediate purposes of this program are (1) to derive the X-ray flux and luminosity after its last outburst in 2011, (2) to diagnose plasma temperature deeply, and (3) to obtain the second sample of non-thermal X-ray emission from classical nova remnants. The target is a remarkable newly discovered candidate of cosmic-ray acceleration sites, and a successful detection of non-thermal X-rays provides a new view of cosmic-ray origins. | GALACTIC POINT SOURCES | 4 | C | DAI TAKEI | USA | 7 | AO7 | COSMIC-RAYS FROM MINIATURE SUPERNOVA REMNANTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407048010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '407048010'
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