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 MCG0208 43.0963 -8.5129 42.484335 -8.717227 37.842662 -23.868775 185.55840319 -55.88722126 57.4541 55016.0987037037 2009-07-04 02:22:08 55017.2134722222 2009-07-05 05:07:24 704045010 42.9115 40 42.9435 42.9115 0 42.9195 2 2 0 2 1 0 0 36.7878 36.7878 96.286 5 PROCESSED 57547.7724768518 2016-06-08 18:32:22 55395 2010-07-18 00:00:00 55027.1160532407 2009-07-15 02:47:07 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 041414 We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. EXTRAGALACTIC COMPACT SOURCES 7 A EZEQUIEL TREISTER USA 4 AO4 THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704045010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '704045010'

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