Comparing XRISM cluster velocity dispersions with predictions from cosmological simulations: are feedback models too ejective?
Authors
XRISM Collaboration
Marc Audard
Hisamitsu Awaki
Ralf Ballhausen
Aya Bamba
Ehud Behar
Rozenn Boissay-Malaquin
Laura Brenneman
Gregory V. Brown
Lia Corrales
Elisa Costantini
Renata Cumbee
Maria Diaz Trigo
Chris Done
Tadayasu Dotani
Ken Ebisawa
Megan E. Eckart
Dominique Eckert
Satoshi Eguchi
Teruaki Enoto
Yuichiro Ezoe
Adam Foster
Ryuichi Fujimoto
Yutaka Fujita
Yasushi Fukazawa
Kotaro Fukushima
Akihiro Furuzawa
Luigi Gallo
Javier A. García
Liyi Gu
Matteo Guainazzi
Kouichi Hagino
Kenji Hamaguchi
Isamu Hatsukade
Katsuhiro Hayashi
Takayuki Hayashi
Natalie Hell
Edmund Hodges-Kluck
Ann Hornschemeier
Yuto Ichinohe
Daiki Ishi
Manabu Ishida
Kumi Ishikawa
Yoshitaka Ishisaki
Jelle Kaastra
Timothy Kallman
Erin Kara
Satoru Katsuda
Yoshiaki Kanemaru
Richard Kelley
Caroline Kilbourne
Shunji Kitamoto
Shogo Kobayashi
Takayoshi Kohmura
Aya Kubota
Maurice Leutenegger
Michael Loewenstein
Yoshitomo Maeda
Maxim Markevitch
Hironori Matsumoto
Kyoko Matsushita
Dan McCammon
Brian McNamara
François Mernier
Eric D. Miller
Jon M. Miller
Ikuyuki Mitsuishi
Misaki Mizumoto
Tsunefumi Mizuno
Koji Mori
Koji Mukai
Hiroshi Murakami
Richard Mushotzky
Hiroshi Nakajima
Kazuhiro Nakazawa
Jan-Uwe Ness
Kumiko Nobukawa
Masayoshi Nobukawa
Hirofumi Noda
Hirokazu Odaka
Shoji Ogawa
Anna Ogorzałek
Takashi Okajima
Naomi Ota
Stephane Paltani
Robert Petre
Paul Plucinsky
Frederick S. Porter
Katja Pottschmidt
Kosuke Sato
Toshiki Sato
Makoto Sawada
Hiromi Seta
Megumi Shidatsu
Aurora Simionescu
Randall Smith
Hiromasa Suzuki
Andrew Szymkowiak
Hiromitsu Takahashi
Mai Takeo
Toru Tamagawa
Keisuke Tamura
Takaaki Tanaka
Atsushi Tanimoto
Makoto Tashiro
Yukikatsu Terada
Yuichi Terashima
Yohko Tsuboi
Masahiro Tsujimoto
Hiroshi Tsunemi
Takeshi Tsuru
Aysegül Tümer
Hiroyuki Uchida
Nagomi Uchida
Yuusuke Uchida
Hideki Uchiyama
Shutaro Ueda
Yoshihiro Ueda
Shinichiro Uno
Jacco Vink
Shin Watanabe
Brian J. Williams
Satoshi Yamada
Shinya Yamada
Hiroya Yamaguchi
Kazutaka Yamaoka
Noriko Yamasaki
Makoto Yamauchi
Shigeo Yamauchi
Tahir Yaqoob
Tomokage Yoneyama
Tessei Yoshida
Mihoko Yukita
Irina Zhuravleva
Weiguang Cui
Stefano Ettori
Skylar Grayson
Annie Heinrich
Hannah McCall
Dylan Nelson
Nobuhiro Okabe
Yuki Omiya
Arnab Sarkar
Evan Scannapieco
Ming Sun
Keita Tanaka
Nhut Truong
Daniel R. Wik
Congyao Zhang
John ZuHone
Abstract
The dynamics of the intra-cluster medium (ICM), the hot plasma that fills galaxy clusters, are shaped by gravity-driven cluster mergers and feedback from supermassive black holes (SMBH) in the cluster cores. XRISM measurements of ICM velocities in several clusters offer insights into these processes. We compare XRISM measurements for nine galaxy clusters (Virgo, Perseus, Centaurus, Hydra A, PKS\,0745--19, A2029, Coma, A2319, Ophiuchus) with predictions from three state-of-the-art cosmological simulation suites, TNG-Cluster, The Three Hundred Project GADGET-X, and GIZMO-SIMBA, that employ different models of feedback. In cool cores, XRISM reveals systematically lower velocity dispersions than the simulations predict, with all ten measurements below the median simulated values by a factor $1.5-1.7$ on average and all falling within the bottom $10\%$ of the predicted distributions. The observed kinetic-to-total pressure ratio is also lower, with a median value of $2.2\%$, compared to the predicted $5.0-6.5\%$ for the three simulations. Outside the cool cores and in non-cool-core clusters, simulations show better agreement with XRISM measurements, except for the outskirts of the relaxed, cool-core cluster A2029, which exhibits an exceptionally low kinetic pressure support ($<1\%$), with none of the simulated systems in either of the three suites reaching such low levels. The non-cool-core Coma and A2319 exhibit dispersions at the lower end but within the simulated spread. Our comparison suggests that the three numerical models may overestimate the kinetic effects of SMBH feedback in cluster cores. Additional XRISM observations of non-cool-core clusters will clarify if there is a systematic tension in the gravity-dominated regime as well.
