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 Q0142-100 26.3171 -9.7556 25.697719 -10.005838 20.677718 -19.226515 161.63610788 -68.48152364 68.9469 56854.9601041667 2014-07-16 23:02:33 56856.4794328704 2014-07-18 11:30:23 709019010 60.9751 55 60.9831 60.9831 0 60.9751 2 2 0 2 1 0 0 10.53 10.53 22.736 0 PROCESSED 57615.4077083333 2016-08-15 09:47:06 57261 2015-08-27 00:00:00 56895.341412037 2014-08-26 08:11:38 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 091431 The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. EXTRAGALACTIC COMPACT SOURCES 7 B BIN CHEN USA 9 AO9 CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709019010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '709019010'

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