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 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'

Your request has been accepted.
The download will start soon automatically.

Go to top of this page ⏏