TY - JOUR
T1 - Design and performance of Soft Gamma-ray Detector onboard the Hitomi (ASTRO-H) satellite
AU - Tajima, Hiroyasu
AU - Watanabe, Shin
AU - Fukazawa, Yasushi
AU - Blandford, Roger
AU - Enoto, Teruaki
AU - Goldwurm, Andrea
AU - Hagino, Kouichi
AU - Hayashi, Katsuhiro
AU - Ichinohe, Yuto
AU - Kataoka, Jun
AU - Katsuta, Junichiro
AU - Kitaguchi, Takao
AU - Kokubun, Motohide
AU - Laurent, Philippe
AU - Lebrun, François
AU - Limousin, Olivier
AU - Madejski, Grzegorz M.
AU - Makishima, Kazuo
AU - Mizuno, Tsunefumi
AU - Mori, Kunishiro
AU - Nakamori, Takeshi
AU - Nakano, Toshio
AU - Nakazawa, Kazuhiro
AU - Noda, Hirofumi
AU - Odaka, Hirokazu
AU - Ohno, Masanori
AU - Ohta, Masayuki
AU - Saito, Shinya
AU - Sato, Goro
AU - Sato, Rie
AU - Takeda, Shinichiro
AU - Takahashi, Hiromitsu
AU - Takahashi, Tadayuki
AU - Tanaka, Takaaki
AU - Tanaka, Yasuyuki
AU - Terada, Yukikatsu
AU - Uchiyama, Hideki
AU - Uchiyama, Yasunobu
AU - Yamaoka, Kazutaka
AU - Yatsu, Yoichi
AU - Yonetoku, Daisuke
AU - Yuasa, Takayuki
N1 - Funding Information:
We greatly appreciate the dedicated work by all students in participating institutions. We thank all the JAXA members who have contributed to the Hitomi (ASTRO-H) project. We acknowledge support from JSPS/MEXT KAKENHI Grant Nos. 16J02333, 24105007, 24244014, 25287059, and 26800160 and the JSPS Core-to-Core Program. All U.S. members gratefully acknowledge support through the NASA Science Mission Directorate. Stanford and SLAC members acknowledge support via DoE contract to SLAC National Accelerator Laboratory DE-AC3-76SF00515 and NASA Grant No. NNX15AM19G. Part of this work was performed under the auspices of the U.S. DoE by LLNL under Contract No. DE-AC52-07NA27344 and also supported by NASA grants to LLNL. Support from the European Space Agency is gratefully acknowledged. French members acknowledge support from the Centre National d’Études Spatiales. We thank contributions by many companies, including in particular, Mitsubishi Heavy Industries, NEC, Hamamatsu Photonics, Acrorad, Ideas, SUPER RESIN, and OKEN.
Publisher Copyright:
© 2018 BMJ Publishing Group Ltd (unless otherwise stated in the text of the article). All rights reserved.
PY - 2018/4/1
Y1 - 2018/4/1
N2 - Hitomi (ASTRO-H) was the sixth Japanese X-ray satellite that carried instruments with exquisite energy resolution of <7 eV and broad energy coverage of 0.3 to 600 keV. The Soft Gamma-ray Detector (SGD) was the Hitomi instrument that observed the highest energy band (60 to 600 keV). The SGD design achieves a low background level by combining active shields and Compton cameras where Compton kinematics is utilized to reject backgrounds coming from outside of the field of view. A compact and highly efficient Compton camera is realized using a combination of silicon and cadmium telluride semiconductor sensors with a good energy resolution. Compton kinematics also carries information for gamma-ray polarization, making the SGD an excellent polarimeter. Following several years of development, the satellite was successfully launched on February 17, 2016. After proper functionality of the SGD components were verified, the nominal observation mode was initiated on March 24, 2016. The SGD observed the Crab Nebula for approximately two hours before the spacecraft ceased to function on March 26, 2016. We present concepts of the SGD design followed by detailed description of the instrument and its performance measured on ground and in orbit.
AB - Hitomi (ASTRO-H) was the sixth Japanese X-ray satellite that carried instruments with exquisite energy resolution of <7 eV and broad energy coverage of 0.3 to 600 keV. The Soft Gamma-ray Detector (SGD) was the Hitomi instrument that observed the highest energy band (60 to 600 keV). The SGD design achieves a low background level by combining active shields and Compton cameras where Compton kinematics is utilized to reject backgrounds coming from outside of the field of view. A compact and highly efficient Compton camera is realized using a combination of silicon and cadmium telluride semiconductor sensors with a good energy resolution. Compton kinematics also carries information for gamma-ray polarization, making the SGD an excellent polarimeter. Following several years of development, the satellite was successfully launched on February 17, 2016. After proper functionality of the SGD components were verified, the nominal observation mode was initiated on March 24, 2016. The SGD observed the Crab Nebula for approximately two hours before the spacecraft ceased to function on March 26, 2016. We present concepts of the SGD design followed by detailed description of the instrument and its performance measured on ground and in orbit.
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U2 - 10.1117/1.JATIS.4.2.021411
DO - 10.1117/1.JATIS.4.2.021411
M3 - Article
AN - SCOPUS:85046023600
SN - 2329-4124
VL - 4
JO - Journal of Astronomical Telescopes, Instruments, and Systems
JF - Journal of Astronomical Telescopes, Instruments, and Systems
IS - 2
M1 - 021411
ER -