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 | 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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