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arxiv 1712.05407 v1 pith:3CO4WIIX submitted 2017-12-14 astro-ph.HE

Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi

Hitomi Collaboration: Felix Aharonian , Hiroki Akamatsu , Fumie Akimoto , Steven W. Allen , Lorella Angelini , Marc Audard , Hisamitsu Awaki , Magnus Axelsson
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Aya Bamba Marshall W. Bautz Roger Blandford Laura W. Brenneman Gregory V. Brown Esra Bulbul Edward M. Cackett Maria Chernyakova Meng P. Chiao Paolo S. Coppi Elisa Costantini Jelle de Plaa Cor P. de Vries Jan-Willem den Herder Chris Done Tadayasu Dotani Ken Ebisawa Megan E. Eckart Teruaki Enoto Yuichiro Ezoe Andrew C. Fabian Carlo Ferrigno Adam R. Foster Ryuichi Fujimoto Yasushi Fukazawa Akihiro Furuzawa Massimiliano Galeazzi Luigi C. Gallo Poshak Gandhi Margherita Giustini Andrea Goldwurm Liyi Gu Matteo Guainazzi Yoshito Haba Kouichi Hagino Kenji Hamaguchi Ilana M. Harrus Isamu Hatsukade Katsuhiro Hayashi Takayuki Hayashi Kiyoshi Hayashida Natalie Hell Junko S. Hiraga Ann Hornschemeier Akio Hoshino John P. Hughes Yuto Ichinohe Ryo Iizuka Hajime Inoue Yoshiyuki Inoue Manabu Ishida Kumi Ishikawa Yoshitaka Ishisaki Masachika Iwai Jelle Kaastra Tim Kallman Tsuneyoshi Kamae Jun Kataoka Satoru Katsuda Nobuyuki Kawai Richard L. Kelley Caroline A. Kilbourne Takao Kitaguchi Shunji Kitamoto Tetsu Kitayama Takayoshi Kohmura Motohide Kokubun Katsuji Koyama Shu Koyama Peter Kretschmar Hans A. Krimm Aya Kubota Hideyo Kunieda Philippe Laurent Shiu-Hang Lee Maurice A. Leutenegger Olivier Limousin Michael Loewenstein Knox S. Long David Lumb Greg Madejski Yoshitomo Maeda Daniel Maier Kazuo Makishima Maxim Markevitch Hironori Matsumoto Kyoko Matsushita Dan McCammon Brian R. McNamara Missagh Mehdipour Eric D. Miller Jon M. Miller Shin Mineshige Kazuhisa Mitsuda Ikuyuki Mitsuishi Takuya Miyazawa Tsunefumi Mizuno Hideyuki Mori Koji Mori Koji Mukai Hiroshi Murakami Richard F. Mushotzky Takao Nakagawa Hiroshi Nakajima Takeshi Nakamori Shinya Nakashima Kazuhiro Nakazawa Kumiko K. Nobukawa Masayoshi Nobukawa Hirofumi Noda Hirokazu Odaka Takaya Ohashi Masanori Ohno Takashi Okajima Naomi Ota Masanobu Ozaki Frits Paerels St\'ephane Paltani Robert Petre Ciro Pinto Frederick S. Porter Katja Pottschmidt Christopher S. Reynolds Samar Safi-Harb Shinya Saito Kazuhiro Sakai Toru Sasaki Goro Sato Kosuke Sato Rie Sato Makoto Sawada Norbert Schartel Peter J. Serlemtsos Hiromi Seta Megumi Shidatsu Aurora Simionescu Randall K. Smith Yang Soong {\L}ukasz Stawarz Yasuharu Sugawara Satoshi Sugita Andrew Szymkowiak Hiroyasu Tajima Hiromitsu Takahashi Tadayuki Takahashi Shin'ichiro Takeda Yoh Takei Toru Tamagawa Takayuki Tamura Takaaki Tanaka Yasuo Tanaka Yasuyuki T. Tanaka Makoto S. Tashiro Yuzuru Tawara Yukikatsu Terada Yuichi Terashima Francesco Tombesi Hiroshi Tomida Yohko Tsuboi Masahiro Tsujimoto Hiroshi Tsunemi Takeshi Go Tsuru Hiroyuki Uchida Hideki Uchiyama Yasunobu Uchiyama Shutaro Ueda Yoshihiro Ueda Shin'ichiro Uno C. Megan Urry Eugenio Ursino Shin Watanabe Norbert Werner Dan R. Wilkins Brian J. Williams Shinya Yamada Hiroya Yamaguchi Kazutaka Yamaoka Noriko Y. Yamasaki Makoto Yamauchi Shigeo Yamauchi Tahir Yaqoob Yoichi Yatsu Daisuke Yonetoku Irina Zhuravleva Abderahmen Zoghbi A. J. J. Raassen
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classification astro-ph.HE
keywords atomicmodelinghitomiapecastrophysicalclustercodescollisional
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The Hitomi SXS spectrum of the Perseus cluster, with $\sim$5 eV resolution in the 2-9 keV band, offers an unprecedented benchmark of the atomic modeling and database for hot collisional plasmas. It reveals both successes and challenges of the current atomic codes. The latest versions of AtomDB/APEC (3.0.8), SPEX (3.03.00), and CHIANTI (8.0) all provide reasonable fits to the broad-band spectrum, and are in close agreement on best-fit temperature, emission measure, and abundances of a few elements such as Ni. For the Fe abundance, the APEC and SPEX measurements differ by 16%, which is 17 times higher than the statistical uncertainty. This is mostly attributed to the differences in adopted collisional excitation and dielectronic recombination rates of the strongest emission lines. We further investigate and compare the sensitivity of the derived physical parameters to the astrophysical source modeling and instrumental effects. The Hitomi results show that an accurate atomic code is as important as the astrophysical modeling and instrumental calibration aspects. Substantial updates of atomic databases and targeted laboratory measurements are needed to get the current codes ready for the data from the next Hitomi-level mission.

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