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".

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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 MRK 509 311.0469 -10.7401 310.365769 -10.921688 310.545768 7.110758 35.95684044 -29.86794514 252.3716 55521.595625 2010-11-21 14:17:42 55523.8155092593 2010-11-23 19:34:20 705025010 102.1205 100 102.1285 102.1285 0 102.1205 2 2 0 2 1 0 0 92.0625 92.0625 191.7697 0 PROCESSED 57554.2039930556 2016-06-15 04:53:45 55916 2011-12-21 00:00:00 55550.2628356482 2010-12-20 06:18:29 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 050113 We propose the observation of one of the typical Seyferts I Mrk 509 for 100 ksec to understand how a vry hard component component that varies independently of power-law is created and how the physical structure near SMBH in Seyferts is. The hard component has been found by carrying out timing analysis of hard X-ray band to explain the extremely broad iron line feature of several Seyferts. Taking this component into account, we succeeded to explain the data of MCG 6-30-15 without the extremely broad iron line, though the origin of this component has not been identified yet. Because Mrk 509 has strong flux and large amplitude of hard X-ray variation, we found it is the most suitable object to verify this component and to get alternative interpretation to the extremely broad iron line. EXTRAGALACTIC COMPACT SOURCES 7 C HIROFUMI NODA JAP 5 AO5 VERIFICATION OF A HARD COMPONENT THAT VARIES INDEPENDENTLY OF POWER-LAW IN TYPE I SEYFERT MRK 509 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705025010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '705025010'

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