Soft X-ray Imager aboard Hitomi (ASTRO-H)

Takaaki Tanaka; Hiroyuki Uchida; Hiroshi Nakajima; Hiroshi Tsunemi; Kiyoshi Hayashida; Takeshi Go Tsuru; Tadayasu Dotani; Ryo Nagino; Shota Inoue; Shuhei Katada; Ryosaku Washino; Masanobu Ozaki; Hiroshi Tomida; Chikara Natsukari; Shutaro Ueda; Masachika Iwai; Koji Mori; Makoto Yamauchi; Isamu Hatsukade; Yusuke Nishioka; Eri Isoda; Masayoshi Nobukawa; Junko S. Hiraga; Takayoshi Kohmura; Hiroshi Murakami; Kumiko K. Nobukawa; Aya Bamba; John P. Doty

doi:10.1117/1.JATIS.4.1.011211

14 February 2018 Soft X-ray Imager aboard Hitomi (ASTRO-H)

Takaaki Tanaka, Hiroyuki Uchida, Hiroshi Nakajima, Hiroshi Tsunemi, Kiyoshi Hayashida, Takeshi Go Tsuru, Tadayasu Dotani, Ryo Nagino, Shota Inoue, Shuhei Katada, Ryosaku Washino, Masanobu Ozaki, Hiroshi Tomida, Chikara Natsukari, Shutaro Ueda, Masachika Iwai, Koji Mori, Makoto Yamauchi, Isamu Hatsukade, Yusuke Nishioka, Eri Isoda, Masayoshi Nobukawa, Junko S. Hiraga, Takayoshi Kohmura, Hiroshi Murakami, Kumiko K. Nobukawa, Aya Bamba, John P. Doty

Author Affiliations +

Journal of Astronomical Telescopes, Instruments, and Systems, Vol. 4, Issue 1, 011211 (February 2018). https://doi.org/10.1117/1.JATIS.4.1.011211

Abstract

The Soft X-ray Imager (SXI) is an imaging spectrometer using charge-coupled devices (CCDs) aboard the Hitomi x-ray observatory. The SXI sensor has four CCDs with an imaging area size of 31 mm×31 mm arranged in a 2×2 array. Combined with the x-ray mirror, the Soft X-ray Telescope, the SXI detects x-rays between 0.4 and 12 keV and covers a 38′×38′ field of view. The CCDs are P-channel fully depleted, back-illumination type with a depletion layer thickness of 200 μm. Low operation temperature down to −120°C as well as charge injection is employed to reduce the charge transfer inefficiency (CTI) of the CCDs. The functionality and performance of the SXI are verified in on-ground tests. The energy resolution measured is 161 to 170 eV in full width at half maximum for 5.9-keV x-rays. In the tests, we found that the CTI of some regions is significantly higher. A method is developed to properly treat the position-dependent CTI. Another problem we found is pinholes in the Al coating on the incident surface of the CCDs for optical light blocking. The Al thickness of the contamination blocking filter is increased to sufficiently block optical light.

CC BY: © The Authors. Published by SPIE under a Creative Commons Attribution 4.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

Citation Download Citation

Takaaki Tanaka, Hiroyuki Uchida, Hiroshi Nakajima, Hiroshi Tsunemi, Kiyoshi Hayashida, Takeshi Go Tsuru, Tadayasu Dotani, Ryo Nagino, Shota Inoue, Shuhei Katada, Ryosaku Washino, Masanobu Ozaki, Hiroshi Tomida, Chikara Natsukari, Shutaro Ueda, Masachika Iwai, Koji Mori, Makoto Yamauchi, Isamu Hatsukade, Yusuke Nishioka, Eri Isoda, Masayoshi Nobukawa, Junko S. Hiraga, Takayoshi Kohmura, Hiroshi Murakami, Kumiko K. Nobukawa, Aya Bamba, and John P. Doty "Soft X-ray Imager aboard Hitomi (ASTRO-H)," Journal of Astronomical Telescopes, Instruments, and Systems 4(1), 011211 (14 February 2018). https://doi.org/10.1117/1.JATIS.4.1.011211

Received: 7 July 2017; Accepted: 19 January 2018; Published: 14 February 2018

ACCESS THE FULL ARTICLE

JOURNAL ARTICLE
15 PAGES

DOWNLOAD PAPER SAVE TO MY LIBRARY