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 1822-37 | 276.4461 | -37.1042 | 275.595774 | -37.133404 | 275.279951 | -13.781506 | 356.85149319 | -11.29112534 | 258.4537 | 54010.4563888889 | 2006-10-02 10:57:12 | 54011.5189699074 | 2006-10-03 12:27:19 | 401051010 | 37.7434 | 40 | 37.7682 | 37.7682 | 37.7434 | 37.7434 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33.1785 | 33.1785 | 91.8059 | 0 | PROCESSED | 57535.7615393518 | 2016-05-27 18:16:37 | 54695 | 2008-08-17 00:00:00 | 54024.6539814815 | 2006-10-16 15:41:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011121 | We propose a 40 ks observation of the accretion disk corona source 4U 1822-37. Despite repeated observations over the years and even excellent high-resolution data from the Chandra Observatory, the nature and origin of the corona and even the source of the Fe K fluorescence emission remains controversial. The spectral resolution of the XIS and the broad-band coverage provided by the combined XIS and HXD instruments make Suzaku uniquely suited to a definitive measurement. Determining the physical conditions in this source is particularly interesting. Because of its geometry 4U 1822-37 is a link between x-ray binaries and AGN, and an therefore serve as a laboratory for studying accretion processes throughout the universe. | GALACTIC POINT SOURCES | 4 | B | JEAN COTTAM | USA | 1 | AO1 | ACCRETION PHYSICS IN THE ADC SOURCE 4U 1822-37 | XIS | Y | https://darts.isas.jaxa.jp/pub/suzaku/ver3.0/401051010/ | Quick Look | ![]() |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '401051010'
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