Measurements of resonant scattering in the Perseus cluster core with Hitomi SXS
Creators: name: Hitomi Collaboration
name: Aharonian, Felix
name: Akamatsu, Hiroki
name: Akimoto, Fumie
name: Allen, Steven W.
name: Angelini, Lorella
name: Audard, Marc
name: Awaki, Hisamitsu
name: Axelsson, Magnus
name: Bamba, Aya
name: Bautz, Marshall W.
name: Blandford, Roger
name: Brenneman, Laura W.
name: Brown, Greg V.
name: Bulbul, Esra
name: Cackett, Edward M.
name: Chernyakova, Maria
name: Chiao, Meng P.
name: Coppi, Paolo S.
name: Costantini, Elisa
name: de Plaa, Jelle
name: de Vries, Cor P.
name: Herder, Jan-Willem den
name: Done, Chris
name: Dotani, Tadayasu
name: Ebisawa, Ken
name: Eckart, Megan E.
name: Enoto, Teruaki
name: Ezoe, Yuichiro
name: Fabian, Andrew C.
name: Ferrigno, Carlo
name: Foster, Adam R.
name: Fujimoto, Ryuichi
name: Fukazawa, Yasushi
name: Furuzawa, Akihiro
name: Galeazzi, Massimiliano
name: Gallo, Luigi C.
name: Gandhi, Poshak
name: Giustini, Margherita
name: Goldwurm, Andrea
name: Gu, Liyi
name: Guainazzi, Matteo
name: Haba, Yoshito
name: Hagino, Kouichi
name: Hamaguchi, Kenji
name: Harrus, Ilana M.
name: Hatsukade, Isamu
name: Hayashi, Katsuhiro
name: Hayashi, Takayuki
name: Hayashida, Kiyoshi
name: Hiraga, Junko S.
name: Hornschemeier, Ann
name: Hoshino, Akio
name: Hughes, John P.
name: Ichinohe, Yuto
name: Iizuka, Ryo
name: Inoue, Hajime
name: Inoue, Yoshiyuki
name: Ishida, Manabu
name: Ishikawa, Kumi
name: Ishisaki, Yoshitaka
name: Kaastra, Jelle
name: Kallman, Tim
name: Kamae, Tsuneyoshi
name: Kataoka, Jun
name: Katsuda, Satoru
name: Kawai, Nobuyuki
name: Kelley, Richard L.
name: Kilbourne, Caroline A.
name: Kitaguchi, Takao
name: Kitamoto, Shunji
name: Kitayama, Tetsu
name: Kohmura, Takayoshi
name: Kokubun, Motohide
name: Koyama, Katsuji
name: Koyama, Shu
name: Kretschmar, Peter
name: Krimm, Hans A.
name: Kubota, Aya
name: Kunieda, Hideyo
name: Laurent, Philippe
name: Lee, Shiu-Hang
name: Leutenegger, Maurice A.
name: Limousin, Olivier O.
name: Loewenstein, Michael
name: Long, Knox S.
name: Lumb, David
name: Madejski, Greg
name: Maeda, Yoshitomo
name: Maier, Daniel
name: Makishima, Kazuo
name: Markevitch, Maxim
name: Matsumoto, Hironori
name: Matsushita, Kyoko
name: McCammon, Dan
name: McNamara, Brian R.
name: Mehdipour, Missagh
name: Miller, Eric D.
name: Miller, Jon M.
name: Mineshige, Shin
name: Mitsuda, Kazuhisa
name: Mitsuishi, Ikuyuki
name: Miyazawa, Takuya
name: Mizuno, Tsunefumi
name: Mori, Hideyuki
name: Mori, Koji
name: Mukai, Koji
name: Murakami, Hiroshi
name: Mushotzky, Richard F.
name: Nakagawa, Takao
name: Nakajima, Hiroshi
name: Nakamori, Takeshi
name: Nakashima, Shinya
name: Nakazawa, Kazuhiro
name: Nobukawa, Kumiko K.
name: Nobukawa, Masayoshi
name: Noda, Hirofumi
name: Odaka, Hirokazu
name: Ohashi, Takaya
name: Ohno, Masanori
name: Okajima, Takashi
name: Ota, Naomi
name: Ozaki, Masanobu
name: Paerels, Frits
name: Paltani, Stephane
name: Petre, Robert
name: Pinto, Ciro
name: Porter, Frederick S.
name: Pottschmidt, Katja
name: Reynolds, Christopher S.
name: Safi-Harb, Samar
name: Saito, Shinya
name: Sakai, Kazuhiro
name: Sasaki, Toru
name: Sato, Goro
name: Sato, Kosuke
name: Sato, Rie
name: Sato, Toshiki
name: Sawada, Makoto
name: Schartel, Norbert
name: Serlemtsos, Peter J.
name: Seta, Hiromi
name: Shidatsu, Megumi
name: Simionescu, Aurora
name: Smith, Randall K.
name: Soong, Yang
name: Stawarz, Lukasz
name: Sugawara, Yasuharu
name: Sugita, Satoshi
name: Szymkowiak, Andrew
name: Tajima, Hiroyasu
name: Takahashi, Hiromitsu
name: Takahashi, Tadayuki
name: Takeda, Shinichiro
name: Takei, Yoh
name: Tamagawa, Toru
name: Tamura, Takayuki
name: Tanaka, Takaaki
name: Tanaka, Yasuo
name: Tanaka, Yasuyuki T.
name: Tashiro, Makoto S.
name: Tawara, Yuzuru
name: Terada, Yukikatsu
name: Terashima, Yuichi
name: Tombesi, Francesco
name: Tomida, Hiroshi
name: Tsuboi, Yohko
name: Tsujimoto, Masahiro
name: Tsunemi, Hiroshi
name: Tsuru, Takeshi Go
name: Uchida, Hiroyuki
name: Uchiyama, Hideki
name: Uchiyama, Yasunobu
name: Ueda, Shutaro
name: Ueda, Yoshihiro
name: Uno, Shinichiro
name: Urry, C. Megan
name: Ursino, Eugenio
name: Watanabe, Shin
name: Werner, Norbert
name: Wilkins, Dan R.
name: Williams, Brian J.
name: Yamada, Shinya
name: Yamaguchi, Hiroya
name: Yamaoka, Kazutaka
name: Yamasaki, Noriko Y.
name: Yamauchi, Makoto
name: Yamauchi, Shigeo
name: Yaqoob, Tahir
name: Yatsu, Yoichi
name: Yonetoku, Daisuke
name: Zhuravleva, Irina
name: Zoghbi, Abderahmen
name: Furukawa, Maki
name: Ogorzalek, Anna
Publisher: name: arXiv
Year: 2017
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: Thanks to its high spectral resolution (~5 eV at 6 keV), the Soft X-ray Spectrometer (SXS) on board Hitomi enables us to measure the detailed structure of spatially resolved emission lines from highly ionized ions in galaxy clusters for the first time. In this series of papers, using the SXS we have measured the velocities of gas motions, metallicities and the multi-temperature structure of the gas in the core of the Perseus cluster. Here, we show that when inferring physical properties from line emissivities in systems like Perseus, the resonant scattering (RS) effect should be taken into account. In the Hitomi waveband, RS mostly affects the FeXXV He$α$ line ($w$) - the strongest line in the spectrum. The flux measured by Hitomi in this line is suppressed by a factor ~1.3 in the inner ~30 kpc, compared to predictions for an optically thin plasma; the suppression decreases with the distance from the center. The $w$ line also appears slightly broader than other lines from the same ion. The observed distortions of the $w$ line flux, shape and distance dependence are all consistent with the expected effect of the resonant scattering in the Perseus core. By measuring the ratio of fluxes in optically thick ($w$) and thin (FeXXV forbidden, He$β$, Ly$α$) lines, and comparing these ratios with predictions from Monte Carlo radiative transfer simulations, the velocities of gas motions have been obtained. The results are consistent with the direct measurements of gas velocities from line broadening described elsewhere in this series, although the systematic and statistical uncertainties remain significant. Further improvements in the predictions of line emissivities in plasma models, and deeper observations with future X-ray missions will enable RS measurements to provide powerful constraints on the amplitude and anisotropy of clusters gas motions.
description: 30 pages, 17 figure, 6 tables, accepted for publication in PASJ