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 | AKN 564 | 340.6246 | 29.7785 | 340.037211 | 29.516371 | 355.343017 | 34.767845 | 92.13720271 | -25.27363853 | 56.6178 | 54277.5375694444 | 2007-06-26 12:54:06 | 54279.8002199074 | 2007-06-28 19:12:19 | 702117010 | 99.9781 | 100 | 99.9861 | 99.9861 | 0 | 99.9781 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87.2253 | 87.2253 | 195.4739 | 1 | PROCESSED | 57539.0843518518 | 2016-05-31 02:01:28 | 54703 | 2008-08-25 00:00:00 | 54333.5152199074 | 2007-08-21 12:21:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022024 | Narrow Line Seyfert 1 galaxies show complex X-ray behaviour. At low flux levels their 2-10~keV spectra are hard, with a huge excess at lower energies. Conversely, at high fluxes, the same objects show a soft 2-10 keV spectrum, with moderate soft excess. This behaviour can be explained either by reflection or absorption models. It is important to distinguish between these scenarios as they imply critical differences in the inferred physics of the accretion flow. There is already good Suzaku data on the hard 2-10 keV spectra from a GT observation of NGC4051. We propose to compare this with 100ks of data from Akn564, the brightest NLS1 at 10keV having a soft 2-10keV spectrum, so as to use the full range of spectral behaviour seen in NLS1's to determine the origin of the soft excess. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHRIS DONE | EUR | 2 | AO2 | UNDERSTANDING THE ORIGIN OF SPECTRAL COMPLEXITY IN NLS1: AKN564 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702117010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '702117010'
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