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 | NGC 3660 | 170.883 | -8.6561 | 170.2492 | -8.381454 | 175.088091 | -11.559037 | 269.10006798 | 48.35629614 | 109.6283 | 56624.1463773148 | 2013-11-28 03:30:47 | 56627.0001967593 | 2013-12-01 00:00:17 | 708043010 | 124.7774 | 120 | 124.7854 | 124.7854 | 0 | 124.7774 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109.7692 | 109.7692 | 246.5434 | 2 | PROCESSED | 57613.5216550926 | 2016-08-13 12:31:11 | 57058 | 2015-02-05 00:00:00 | 56691.7534953704 | 2014-02-03 18:05:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082003 | We propose a 120-ks observation of NGC 3660, which is a strong candidate for a True Seyfert 2, a Seyfert that intrinsically lacks the broad line regions (BLRs), and challenges the AGN unified scheme. However, a puzzling BeppoSAX observation lingers, which shows excess emission above 10 keV indicative of a Compton thick AGN. Nevertheless, rapid variability below 10 keV and meagre iron line emission (EW=60 eV) strongly argue against this conclusion. Data from the HXD will elucidate the situation, and either dispel this evidence, adding weight to the True Seyfert 2 scenario, or confirm the presence of heavily obscured emission, which may be explained by a partial covering scenario. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MURRAY BRIGHTMAN | EUR | 8 | AO8 | NGC 3660: A TRUE SEYFERT 2? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708043010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '708043010'
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