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 | MARKARIAN 509 | 311.0194 | -10.6637 | 310.338544 | -10.845188 | 310.53976 | 7.19158 | 36.02321332 | -29.81091499 | 73.1708 | 53850.7831481482 | 2006-04-25 18:47:44 | 53851.5252199074 | 2006-04-26 12:36:19 | 701093010 | 24.5756 | 25 | 24.5756 | 24.5756 | 24.5916 | 24.5916 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 15.407 | 15.407 | 64.0979 | 1 | PROCESSED | 57533.5586342593 | 2016-05-25 13:24:26 | 54394 | 2007-10-21 00:00:00 | 53907.6894560185 | 2006-06-21 16:32:49 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GABRIELE PONTI | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '701093010'
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