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 ETA CARINAE 161.3639 -59.6742 160.876523 -59.410706 202.202933 -58.878505 287.63630523 -0.59715454 170.6228 54877.528287037 2009-02-15 12:40:44 54878.4119675926 2009-02-16 09:53:14 403038010 35.5525 30 35.5685 35.5525 0 35.5605 2 2 0 2 1 0 0 31.1193 31.1193 76.3239 1 PROCESSED 57545.5564814815 2016-06-06 13:21:20 55328 2010-05-12 00:00:00 54893.4307407407 2009-03-03 10:20:16 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 031124 X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). GALACTIC POINT SOURCES 4 A KENJI HAMAGUCHI USA 3 AO3 X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM HXD Y https://darts.isas.jaxa.jp/pub/suzaku/ver3.0/403038010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '403038010'

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