Methodology and performance of the two-year galactic plane scanning survey of Insight-HXMT
Methodology and performance of the two-year galactic plane scanning survey of Insight-HXMT
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Insight-HXMT两年银河平面扫描巡天的方法和性能
DOI：
10.1016/j.jheap.2020.02.005
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发表时间：
2020-03
影响因子：
3.8
通讯作者：
et al.
中科院分区：
文献类型：
--
作者：
Sai Na;Liao Jin-Yuan;Li Cheng-Kui;et al.
银河系平面扫描测量是硬X射线调制望远镜(Insight-HXMT)的主要科学目标之一。在两年的运行中，共进行了1000多次扫描观测，完全覆盖了整个银河面(0∘<；L<；360∘，−10∘<；b<；10∘)。总结了Insight-HXMT两年来的银面扫描观测，包括低能望远镜、中能望远镜和高能望远镜的扫描数据特点、数据分析过程和初步结果。利用光曲线PSF拟合法，得到了每一次扫描观测区域内已知源的通量和通量误差。根据信噪比和通量的关系，估算了Insight-HXMT三台望远镜的5个σ灵敏度分别为∼7.6×10−11erg cm−2 S−1(3MCRAB，1−6keV)，∼4.0×10−10erg cm−2 S−1(20MCRAB，7−40keV)和∼2.6×10−10erg cm−2 S−1(18MCRAB，25−100keV)2−3h。截至2019年9月，三台望远镜监测了800多个各类X射线源，获得了它们三个能带的长期光曲线，以便进行进一步的科学分析。
The Galactic plane scanning survey is one of the main scientific objectives of the Hard X-ray Modulation Telescope (known as Insight-HXMT). During the two-year operation of Insight-HXMT, more than 1000 scanning observations have been performed and the whole Galactic plane (0∘< l< 360∘,− 10∘< b< 10∘) has been covered completely. We summarize the Galactic plane scanning survey of Insight-HXMT for two years, including the characteristics of the scanning data, the data analysis process and the preliminary results of the Low-Energy telescope, the Medium-Energy telescope and the High-Energy telescope. With the light curve PSF fitting method, the fluxes of the known sources in the scanned area as well as the flux errors are obtained for each scanning observation. From the relationships of SNRs and fluxes, the 5σ sensitivities of three telescopes of Insight-HXMT are estimated as∼ 7.6× 10− 11 erg cm− 2 s− 1 (3 mCrab, 1− 6 keV),∼ 4.0× 10− 10 erg cm− 2 s− 1 (20 mCrab, 7− 40 keV) and∼ 2.6× 10− 10 erg cm− 2 s− 1 (18 mCrab, 25− 100 keV) for an individual scanning observation of 2− 3 h, respectively. Up to September 2019, more than 800 X-ray sources with various types are monitored by the three telescopes and their long-term light curves with three energy bands are obtained to make further scientific analyses.
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影响因子：
1.9
作者：
Md Chand Asique;U. Prasad;M. Hassan;Md Sanam Suraj
通讯作者：
Md Chand Asique;U. Prasad;M. Hassan;Md Sanam Suraj
DOI：
10.1088/0067-0049/220/1/8
发表时间：
2015-04
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
K. Madsen;F. Harrison;C. Markwardt;H. An;B. Grefenstette;M. Bachetti;H. Miyasaka;T. Kitaguchi;V. Bhalerao;S. Boggs;F. Christensen;W. Craig;K. Forster;F. Fuerst;C. Hailey;M. Perri;S. Puccetti;V. Rana;D. Stern;D. Walton;N. Westergaard;Will Zhang
通讯作者：
K. Madsen;F. Harrison;C. Markwardt;H. An;B. Grefenstette;M. Bachetti;H. Miyasaka;T. Kitaguchi;V. Bhalerao;S. Boggs;F. Christensen;W. Craig;K. Forster;F. Fuerst;C. Hailey;M. Perri;S. Puccetti;V. Rana;D. Stern;D. Walton;N. Westergaard;Will Zhang
HXMT/HE 飞行背景模拟
影响因子：
1.9
作者：
谢斐;张娟;宋黎明;熊少林;关菊
通讯作者：
关菊
DOI：
10.1016/0168-583x(88)90063-8
发表时间：
1988-09-01
影响因子：
1.3
作者：
RYAN, CG;CLAYTON, E;COUSENS, DR
通讯作者：
COUSENS, DR
DOI：
10.1088/0067-0049/207/2/19
发表时间：
2012-12
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
W. Baumgartner;J. Tueller;C. Markwardt;G. Skinner;S. Barthelmy;R. Mushotzky;P. Evans;N. Gehrels
通讯作者：
W. Baumgartner;J. Tueller;C. Markwardt;G. Skinner;S. Barthelmy;R. Mushotzky;P. Evans;N. Gehrels