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 3516 | 166.6684 | 72.5566 | 165.815394 | 72.826934 | 123.372761 | 57.969452 | 133.25443095 | 42.40827092 | 314.5458 | 56409.0119560185 | 2013-04-27 00:17:13 | 56409.446087963 | 2013-04-27 10:42:22 | 708006020 | 19.103 | 50 | 19.119 | 19.103 | 0 | 19.119 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 20.2121 | 20.2121 | 30.7239 | 0 | PROCESSED | 57611.1744907407 | 2016-08-11 04:11:16 | 56383 | 2013-04-01 00:00:00 | 56457.6034375 | 2013-06-14 14:28:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006020/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '708006020'
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