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 WR140 305.211 43.8318 304.788544 43.672134 327.46168 60.444795 80.94998516 4.10805919 199.7371 54835.3583449074 2009-01-04 08:36:01 54836.4252199074 2009-01-05 10:12:19 403031010 47.2664 40 47.2664 47.2664 0 47.2824 2 2 0 2 1 0 0 45.303 45.303 92.1618 0 PROCESSED 57545.1036921296 2016-06-06 02:29:19 55328 2010-05-12 00:00:00 54850.2164583333 2009-01-19 05:11:42 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030157 WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. GALACTIC POINT SOURCES 4 A YOSHITOMO MAEDA JAP 3 AO3 X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403031010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '403031010'

Your request has been accepted.
The download will start soon automatically.

Go to top of this page ⏏