DARTS Astro
total 1
Show the used SQL Download WgetScript
No. | target_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 | proposal_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 | hxd_burst_num | processing_status | processing_end_time_mjd | processing_end_time | public_date_mjd | public_date | distribute_start_date_mjd | distribute_start_date | processing_version | processing_quantity | processing_software | proposal_id | proposal_abstract | proposal_category | proposal_category_code | proposal_priority | pi_name | co_pi_name | proposal_affiliated_country | proposal_cycle_count | observation_type | proposal_title | main_detector | xis_injection_flag | data_access_url | ql_access_url | ql_image_url |
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1 | 4U 1705-44 | 257.2313 | -44.1028 | 256.328133 | -44.039108 | 260.196098 | -21.094402 | 343.32206131 | -2.34487049 | 297.0793 | 54014.4242708333 | 2006-10-06 10:10:57 | 54015.0891087963 | 2006-10-07 02:08:19 | 401046030 | 20.065 | 20 | 20.065 | 20.065 | 20.065 | 20.065 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.9196 | 17.9196 | 57.4239 | 2 | PROCESSED | 57535.7945138889 | 2016-05-27 19:04:06 | 54526 | 2008-03-01 00:00:00 | 54021.6765162037 | 2006-10-13 16:14:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | ANDREW YOUNG | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N | https://darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046030/ | Quick Look | ![]() |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '401046030'
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