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 | 4U 0142+61 | 26.5838 | 61.7628 | 25.715895 | 61.512967 | 52.16359 | 46.394147 | 129.37704782 | -0.4200572 | 82.997 | 56504.4205902778 | 2013-07-31 10:05:39 | 56506.6252430556 | 2013-08-02 15:00:21 | 408011010 | 101.1678 | 100 | 101.1678 | 101.1828 | 0 | 101.1828 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.4739 | 102.4739 | 190.4637 | 1 | PROCESSED | 57612.1558680556 | 2016-08-12 03:44:27 | 56953 | 2014-10-23 00:00:00 | 56587.5059606482 | 2013-10-22 12:08:35 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080035 | A toroidal magnetic field is thought to be formed in neutron star interior after core-collapse supernovae and become an energy source with recently observed X-ray outbursts from magnetars. Since the toroidal field is hidden in the stellar interior, it was thought to be undetectable via the well-known p-pdot method and the cyclotron resonance scattering features. However, a magnetic stress of the magnetar toroidal field is strong enough to distort the stellar shape and produce a free precession in its X-ray pulse timing if the emission pattern deviates from its axis of symmetry. From our analyses of magnetar 4U 0142+61, we found an evidence on the free precession in the hard X-ray component. To confirm and establish this evidence, we propose an additional 100 ks observation of 4U 0142+61. | GALACTIC POINT SOURCES | 4 | A | TERUAKI ENOTO | JAP | 8 | AO8 | TOROIDAL FIELD INSIDE MAGNETARS OBSERVED WITH SUZAKU TIMING ANALYSES OF ITS FREE PRECESSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408011010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '408011010'
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