DARTS Astro

total 1

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
1 4U 0142+61 26.4803 61.7944 25.612931 61.544346 52.126454 46.446482 129.32255084 -0.39946076 40.959 54325.1695949074 2007-08-13 04:04:13 54327.5209259259 2007-08-15 12:30:08 402013010 99.6744 100 99.6744 99.6744 0 99.6744 2 2 0 2 1 0 0 101.6096 101.6096 203.1297 4 PROCESSED 57549.823900463 2016-06-10 19:46:25 54730 2008-09-21 00:00:00 54347.6221296296 2007-09-04 14:55:52 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 020058 Recently, high energy pulsed x-ray emissions from anomalous x-ay pulsears have been founded. This emissions extend to neary 100 keV with photon index ~1, and the emission mechanism is unknown. In order to trace this enigmatic component, we propose the observation of the anomalous x-ray pulsar 4u 0142+61 with 100 ksec exposures. The main aim of this observation is to examine how high energy this emission extend to. Because the these emissions are almost 100% pulsed component, so using the pulse on-off method, we can achive the ultimate sensitivity not depending on the reproducibility of the background but depending only on the photon statistics. If the spectrum have the strong break neary ~250 keV, this emissions have originated as the compton scatterd photons in the star surface. GALACTIC POINT SOURCES 4 A TERUAKI ENOTO JAP 2 AO2 THE PULSED HARD X-RAY EMISSION FROM ANOMALOUS X-RAY PULSAR 4U 0142+61 HXD Y https://darts.isas.jaxa.jp/pub/suzaku/ver3.0/402013010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '402013010'

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