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 | MARKARIAN 335 | 1.5539 | 20.2624 | 0.911019 | 19.984083 | 9.744165 | 17.917566 | 108.74842011 | -41.36053721 | 68.4831 | 53907.0624537037 | 2006-06-21 01:29:56 | 53910.7585532407 | 2006-06-24 18:12:19 | 701031010 | 151.2884 | 150 | 151.2964 | 151.2884 | 151.2964 | 151.2964 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 140.9812 | 140.9812 | 319.3028 | 4 | PROCESSED | 57534.8340046296 | 2016-05-26 20:00:58 | 54401 | 2007-10-28 00:00:00 | 53928.5392361111 | 2006-07-12 12:56:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011323 | We propose to observe the two Seyfert 1 galaxies Mrk 335 and ESO198-G024 for a total exposure of 150 ks each with the high sensitivity and broad band coverage of the Suzaku satellite. Both sources show a broad Fe K line and a strong soft excess. One appealing explanation for the nature of the soft excess is reflection. Fundamental to this hypothesis is the assumption that the same self-consistent reflection spectrum explains the Fe K line (including its shape), the soft excess, and also the Compton reflection hump above 20 keV. Suzaku's ability to measure all three reflection components simultaneously enables the different spectral models to be disentangled and reflection to be strongly tested. Understanding black hole accretion is fundamental to NASA's "SEU" theme. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JON MILLER | USA | 1 | AO1 | REVEALING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701031010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '701031010'
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