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 ZETA OPH 249.2878 -10.5628 248.598836 -10.46277 249.217592 11.396196 6.28378927 23.59180747 94.9452 54540.8758912037 2008-03-15 21:01:17 54543.8543287037 2008-03-18 20:30:14 402038010 105.5837 100 105.5917 105.5917 0 105.5837 2 2 0 2 1 0 0 79.9813 79.9813 257.3178 2 PROCESSED 57541.9592708333 2016-06-02 23:01:21 54922 2009-04-01 00:00:00 54553.3785300926 2008-03-28 09:05:05 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 021022 Zeta Oph is a well known optical and UV variable star and is now known to displays both short (hours) and long (years) term X-ray variability. The short term variability has different periods for the soft and hard X-ray bands. The soft period being identical with the UV DAC reoccurrence period. The hard period is 40 percent smaller than the soft period and the source of it's variability is thus far unclear. Zeta Oph has been observed by several X-ray telescopes over a 22 year time span and the observations show significant variations in the total observed X-ray flux. We are requesting an XIS observation of this star to develop: 1) a greater understanding of the hard X-ray emission; 2) confirm the hard and soft periodicities, and; 3) provide further monitoring of the long term variability. GALACTIC POINT SOURCES 4 C WAYNE WALDRON USA 2 AO2 MULTIPLE X-RAY EMISSION PERIODICITY IN THE RAPIDLY ROTATING O-STAR, ZETA OPH XIS Y https://darts.isas.jaxa.jp/pub/suzaku/ver3.0/402038010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '402038010'

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