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 | NGC 2110 | 88.0444 | -7.458 | 87.440268 | -7.468978 | 87.743148 | -30.884192 | 212.92660512 | -16.54877043 | 103.4188 | 53629.3796296296 | 2005-09-16 09:06:40 | 53631.8308333333 | 2005-09-18 19:56:24 | 100024010 | 101.7487 | 100 | 101.9265 | 103.7601 | 101.7487 | 102.1483 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 86.0433 | 86.0433 | 211.7558 | 4 | PROCESSED | 57527.4030324074 | 2016-05-19 09:40:22 | 54247 | 2007-05-27 00:00:00 | 54035.4624189815 | 2006-10-27 11:05:53 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000024 | The Narrow Emission Line Galaxy NGC 2110 was the brightest AGN in the initial BAT survey release (BAT flux of 2.1E-10 erg/cm2/sec) visible to Suzaku during Sept./Oct., and is still currently bright in BAT. A 2003 RXTE observation yielded F_2-10 keV = 4E-11 erg/cm2/sec. The source is currently almost 3 times brighter than during the SAX observations. The main goals are to measure the high energy cutoff and to place a strong limit on the presence of reflection. The Compton reflection hump is weak in SAX data (suggesting that the Fe K line originates in Compton-thin material). Determining the strength of the reflection component is critical for constraining the geometry of the accreting material. | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Narrow Emission Line Galaxy NGC 2110 | N | https://darts.isas.jaxa.jp/pub/suzaku/ver3.0/100024010/ | Quick Look | ![]() |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '100024010'
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