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 CEN X-4 224.5893 -31.6684 223.829289 -31.468804 231.309524 -14.121168 332.24097668 23.88258751 104.6233 54847.9102314815 2009-01-16 21:50:44 54850.9717939815 2009-01-19 23:19:23 403057010 146.6704 150 146.6876 146.6704 0 146.6916 2 2 0 2 1 0 0 133.6185 133.6185 264.4539 2 PROCESSED 57545.3354513889 2016-06-06 08:03:03 55328 2010-05-12 00:00:00 54880.5460069444 2009-02-18 13:06:15 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 031161 Observations of thermal emission from the surface of quiescent neutron star low-mass X-ray binaries (LMXBs) can be used to measure neutron star radii. However, their quiescent spectra are complicated due to the presence of an additional power-law, and because variability has been seen on timescales as short as 100s. The nearest known neutron star LMXB Cen X-4 gives us the clearest view of these objects. But, the best observation so far lacked the sensitivity to determine the cause of the variability. Yet, the cause has important ramifications for measuring neutron star radii - if it is the thermal (rather than power-law) component that is varying our picture of quiescent emission may be wrong. To solve this critical problem we propose a 150 ksec observation of Cen X-4 with Suzaku. GALACTIC POINT SOURCES 4 A EDWARD CACKETT USA 3 AO3 UNCOVERING VARIABLE QUIESCENT EMISSION IN THE NEUTRON STAR CEN X-4 XIS Y https://darts.isas.jaxa.jp/pub/suzaku/ver3.0/403057010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '403057010'

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