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 | 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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