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 RX J1940.1-1025 295.0445 -10.4193 294.356962 -10.535652 295.074294 10.867465 28.98688715 -15.49869645 79.7405 54572.8979976852 2008-04-16 21:33:07 54573.743275463 2008-04-17 17:50:19 403027010 32.4536 30 32.4536 32.4536 0 32.4536 2 2 0 2 1 0 0 26.4657 26.4657 73.0219 2 PROCESSED 57542.3241087963 2016-06-03 07:46:43 54953 2009-05-02 00:00:00 54587.0481481482 2008-05-01 01:09:20 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030140 Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. GALACTIC POINT SOURCES 4 B KEN EBISAWA JAP 3 AO3 IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL XIS Y https://darts.isas.jaxa.jp/pub/suzaku/ver3.0/403027010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '403027010'

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