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 M81 148.8829 69.0533 147.858629 69.290285 119.502258 51.56628 142.10623941 40.90540672 287.1391 57160.4721180556 2015-05-18 11:19:51 57162.9807523148 2015-05-20 23:32:17 710017010 97.7022 100 97.7022 99.738 0 99.7444 3 2 0 2 0 0 0 0 0 0.3 0 PROCESSED 57618.7210532407 2016-08-18 17:18:19 57543 2016-06-04 00:00:00 57177.3710300926 2015-06-04 08:54:17 3.0.22.44 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 102700 We propose to observe the Low-Luminosity Active Galactic Nucleus of M81 for 200 ksec with NuSTAR and for 100 ksec with Suzaku. In low accretion rate AGN, where does the optically thick part of the accretion disk stop? Does it go in to within a few gravitational radii of the black hole, as in higher accretion rate Seyfert galaxies, or does it stop hundreds of gravitational radii from the black hole? Using NuSTAR and Suzaku spectra we will measure the strengths of the Compton reflection hump, Fe K alpha, Fe XXV and Fe XXVI lines. This will determine whether the Fe K alpha line is produced by reflection off the optically thick outer disk, or is produced in the optically thin inner flow. We will measure the reflection fraction and constrain the source geometry and disk transition radius. EXTRAGALACTIC COMPACT SOURCES 7 A ANDREW YOUNG EUR 10 AO10 M81: ACCRETION GEOMETRY AT LOW EDDINGTON RATES XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710017010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '710017010'

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