Hitomi constraints on the 3.5 keV line in the Perseus galaxy cluster

Hitomi Collaboration: Felix A. Aharonian , Hiroki Akamatsu , Fumie Akimoto , Steven W. Allen , Lorella Angelini , Keith A. Arnaud , Marc Audard , Hisamitsu Awaki

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Magnus Axelsson Aya Bamba Marshall W. Bautz Roger D. Blandford Laura W. Brenneman Gregory V. Brown Esra Bulbul Edward M. Cackett Maria Chernyakova Meng P. Chiao Paolo Coppi Elisa Costantini Jelle de Plaa 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 Harrus Isamu Hatsukade Katsuhiro Hayashi Takayuki Hayashi Kiyoshi Hayashida Junko Hiraga Ann E. Hornschemeier Akio Hoshino John P. Hughes Yuto Ichinohe Ryo Iizuka Hajime Inoue Shota Inoue Yoshiyuki Inoue Kazunori Ishibashi Manabu Ishida Kumi Ishikawa Yoshitaka Ishisaki Masayuki Itoh Masachika Iwai Naoko Iyomoto Jelle S. Kaastra Timothy Kallman Tuneyoshi Kamae Erin Kara Jun Kataoka Satoru Katsuda Junichiro Katsuta Madoka Kawaharada Nobuyuki Kawai Richard L. Kelley Dmitry Khangulyan Caroline A. Kilbourne Ashley L. King Takao Kitaguchi Shunji Kitamoto Tetsu Kitayama Takayoshi Kohmura Motohide Kokubun Shu Koyama Katsuji Koyama Peter Kretschmar Hans A. Krimm Aya Kubota Hideyo Kunieda Philippe Laurent Francois Lebrun Shiu-Hang Lee Maurice Leutenegger Olivier Limousin Michael Loewenstein Knox S. Long David Lumb Grzegorz M. 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 Harvey Moseley Koji Mukai Hiroshi Murakami Toshio Murakami Richard F. Mushotzky Takao Nakagawa Hiroshi Nakajima Takeshi Nakamori Toshio Nakano Shinya Nakashima Kazuhiro Nakazawa Kumiko Nobukawa Masayoshi Nobukawa Hirofumi Noda Masaharu Nomachi Steve L. O'Dell Hirokazu Odaka Takaya Ohashi Masanori Ohno Takashi Okajima Naomi Ota Masanobu Ozaki Frits Paerels Stephane Paltani Arvind Parmar Robert Petre Ciro Pinto Martin Pohl F. Scott Porter Katja Pottschmidt Brian D. Ramsey Christopher S. Reynolds Helen R. Russell Samar Safi-Harb Shinya Saito Kazuhiro Sakai Hiroaki Sameshima Toru Sasaki Goro Sato Kosuke Sato Rie Sato Makoto Sawada Norbert Schartel Peter J. Serlemitsos Hiromi Seta Megumi Shidatsu Aurora Simionescu Randall K. Smith Yang Soong Lukasz Stawarz Yasuharu Sugawara Satoshi Sugita Andrew E. Szymkowiak Hiroyasu Tajima Hiromitsu Takahashi Tadayuki Takahashi Shin'ichiro Takeda Yoh Takei Toru Tamagawa Keisuke Tamura Takayuki Tamura Takaaki Tanaka Yasuo Tanaka Yasuyuki Tanaka Makoto Tashiro Yuzuru Tawara Yukikatsu Terada Yuichi Terashima Francesco Tombesi Hiroshi Tomida Yohko Tsuboi Masahiro Tsujimoto Hiroshi Tsunemi Takeshi Tsuru Hiroyuki Uchida Hideki Uchiyama Yasunobu Uchiyama Shutaro Ueda Yoshihiro Ueda Shiro Ueno Shin'ichiro Uno C. Meg Urry Eugenio Ursino Cor P. de Vries Shin Watanabe Norbert Werner Daniel R. Wik 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 Atsumasa Yoshida Irina Zhuravleva Abderahmen Zoghbi

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classification 🌌 astro-ph.HE astro-ph.COastro-ph.GA

keywords linehitomiperseusclusterfaintfindhighreported

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High-resolution X-ray spectroscopy with Hitomi was expected to resolve the origin of the faint unidentified E=3.5 keV emission line reported in several low-resolution studies of various massive systems, such as galaxies and clusters, including the Perseus cluster. We have analyzed the Hitomi first-light observation of the Perseus cluster. The emission line expected for Perseus based on the XMM-Newton signal from the large cluster sample under the dark matter decay scenario is too faint to be detectable in the Hitomi data. However, the previously reported 3.5 keV flux from Perseus was anomalously high compared to the sample-based prediction. We find no unidentified line at the reported high flux level. Taking into account the XMM measurement uncertainties for this region, the inconsistency with Hitomi is at a 99% significance for a broad dark-matter line and at 99.7% for a narrow line from the gas. We do not find anomalously high fluxes of the nearby faint K line or the Ar satellite line that were proposed as explanations for the earlier 3.5 keV detections. We do find a hint of a broad excess near the energies of high-n transitions of Sxvi (E=3.44 keV rest-frame) -- a possible signature of charge exchange in the molecular nebula and another proposed explanation for the unidentified line. While its energy is consistent with XMM pn detections, it is unlikely to explain the MOS signal. A confirmation of this interesting feature has to wait for a more sensitive observation with a future calorimeter experiment.

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Hitomi constraints on the 3.5 keV line in the Perseus galaxy cluster

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