DARTS Astro
total 1
Show the used SQL Download WgetScript
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 |
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1 | KT PER | 24.2933 | 50.9468 | 23.514247 | 50.69234 | 43.593687 | 37.546222 | 130.24865907 | -11.27406186 | 260.9001 | 54843.8957060185 | 2009-01-12 21:29:49 | 54844.5334953704 | 2009-01-13 12:48:14 | 403041010 | 29.1957 | 20 | 29.1957 | 29.1957 | 0 | 29.1957 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.1658 | 28.1658 | 55.0899 | 0 | PROCESSED | 57545.1649537037 | 2016-06-06 03:57:32 | 55328 | 2010-05-12 00:00:00 | 54854.0547916667 | 2009-01-23 01:18:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031144 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates. | GALACTIC POINT SOURCES | 4 | C | KOJI MUKAI | USA | 3 | AO3 | BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3 | XIS | Y | https://darts.isas.jaxa.jp/pub/suzaku/ver3.0/403041010/ | Quick Look | ![]() |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '403041010'
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