Modeling the spectral response for the soft X-ray imager onboard the ASTRO-H satellite

被引:7
作者
Inoue, Shota [1 ,2 ]
Hayashida, Kiyoshi [1 ,2 ]
Katada, Shuhei [1 ,2 ]
Nakajima, Hiroshi [1 ,2 ]
Nagino, Ryo [1 ,2 ]
Anabuki, Naohisa [1 ,2 ]
Tsunemi, Hiroshi [1 ,2 ]
Tsuru, Takeshi Go [3 ]
Tanaka, Takaaki [3 ]
Uchida, Hiroyuki [3 ]
Nobukawa, Masayoshi [4 ,5 ]
Nobukawa, Kumiko Kawabata [3 ]
Washino, Ryosaku [3 ]
Mori, Koji [6 ]
Isoda, Eri [6 ]
Sakata, Miho [6 ]
Kohmura, Takayoshi [7 ]
Tamasawa, Koki [7 ]
Tanno, Shoma [8 ]
Yoshino, Yuma [8 ]
Konno, Takahiro [8 ]
Ueda, Shutaro [9 ]
机构
[1] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyama Cho, Toyonaka, Osaka 5600043, Japan
[2] Osaka Univ, Grad Sch Sci, Project Res Ctr Fundamental Sci, 1-1 Machikaneyama Cho, Toyonaka, Osaka 5600043, Japan
[3] Kyoto Univ, Grad Sch Sci, Dept Phys, Sakyo Ku, Oiwake Cho, Kyoto 6068502, Japan
[4] Nara Univ Educ, Dept Teacher Training, Takabatake Cho, Nara 6308528, Japan
[5] Nara Univ Educ, Sch Educ, Takabatake Cho, Nara 6308528, Japan
[6] Miyazaki Univ, Dept Appl Phys, 1-1 Gakuen Kibana Dai Nishi, Miyazaki 8892192, Japan
[7] Tokyo Univ Sci, Grad Sch Sci & Technol, Dept Phys, 2641 Yamazaki, Noda, Chiba 2780022, Japan
[8] Tokyo Univ Sci, Fac Sci & Technol, Dept Phys, 2641 Yamazaki, Noda, Chiba 2780022, Japan
[9] Japan Aerosp Explorat Agcy JAXA, ISAS, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan
关键词
X-ray; Charge coupled device; P-channel CCD; ASTRO-H; IONIZATION; EMISSION;
D O I
10.1016/j.nima.2016.03.071
中图分类号
TH7 [仪器、仪表];
学科分类号
0804 ; 080401 ; 081102 ;
摘要
The ASTRO-H satellite is the 6th Japanese X-ray astronomical observatory to be launched in early 2016. The satellite carries four kinds of detectors, and one of them is an X-ray CCD camera, the soft X-ray imager (SXI), installed on the focal plane of an X-ray telescope. The SXI contains four CCD chips, each with an imaging area of 31 mm x 31 mm, arrayed in mosaic, covering the field-of-view of 38' x 38', the widest ever flown in orbit. The CCDs are a P-channel back-illuminated (BI) type with a depletion layer thickness of 200 um. We operate the CCDs in a photon counting mode in which the position and energy of each photon are measured in the energy band of 0.4-12 keV. To evaluate the X-ray spectra obtained with the SXI, an accurate calibration of its response function is essential. For this purpose, we performed calibration experiments at Kyoto and Photon Factory of KEK, each with different X-ray sources with various X-ray energies. We fit the obtained spectra with 5 components; primary peak, secondary peak, constant tail, Si escape and Si fluorescence, and then model their energy dependence using physics based or empirical formulae. Since this is the first adoption of P -channel BI -type CCDs on an X-ray astronomical satellite, we need to take special care on the constant tail component which is originated in partial charge collection. It is found that we need to assume a trapping layer at the incident surface of the CCD and implement it in the response model. In addition, the Si fluorescence component of the SXI response is significantly weak, compared with those of front -illuminated type CCDs. (C) 2016 Elsevier B.V. All rights reserved.
引用
收藏
页码:415 / 419
页数:5
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