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 | GRS 1915+105 | 288.7933 | 10.9535 | 288.203422 | 10.865162 | 292.134883 | 32.961388 | 45.37037141 | -0.21130356 | 67.354 | 54227.6113657407 | 2007-05-07 14:40:22 | 54229.0717476852 | 2007-05-09 01:43:19 | 402071010 | 65.6568 | 37 | 65.6568 | 65.8039 | 0 | 65.6728 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 56.8973 | 56.8973 | 126.168 | 1 | PROCESSED | 57538.6640972222 | 2016-05-30 15:56:18 | 54702 | 2008-08-24 00:00:00 | 54235.5321759259 | 2007-05-15 12:46:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021132 | We have discovered a connection between Fe line strength and QPO phase in RXTE observations of GRS 1915+105. This connection independently ties Fe lines to radii less than 100 R_Schw. QPO-phase-resolved Suzaku spectra will enable us to detect changes in the relativistic line profile (inner radius, equivalent width), to extend the connection to the broadband disk reflection spectrum, and to test models for the Fe line - QPO connection. Moreover, at CCD resolution, the connection can be used to over-constrain disk radii - a first step toward mapping the inner disk. We therefore request a 37 ksec TOO observation of GRS 1915+105. Understanding black hole accretion is fundamental to NASA's "SEU" theme. | GALACTIC POINT SOURCES | 4 | A | JON MILLER | USA | 2 | AO2-TOO | THE RELATIVISTIC IRON LINE - QPO CONNECTION IN GRS 1915+105 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402071010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '402071010'
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