title: The bulk motion of gas in the core of the Centaurus galaxy cluster
Creators: name: Audard, Marc
name: Awaki, Hisamitsu
name: Ballhausen, Ralf
name: Bamba, Aya
name: Behar, Ehud
name: Boissay-Malaquin, Rozenn
name: Brenneman, Laura
name: Brown, Gregory V.
name: Corrales, Lia
name: Costantini, Elisa
name: Cumbee, Renata
name: Done, Chris
name: Dotani, Tadayasu
name: Ebisawa, Ken
name: Eckart, Megan E.
name: Eckert, Dominique
name: Enoto, Teruaki
name: Eguchi, Satoshi
name: Ezoe, Yuichiro
name: Foster, Adam
name: Fujimoto, Ryuichi
name: Fujita, Yutaka
name: Fukazawa, Yasushi
name: Fukushima, Kotaro
name: Furuzawa, Akihiro
name: Gallo, Luigi
name: Garc�A, Javier A.
name: Gu, Liyi
name: Guainazzi, Matteo
name: Hagino, Kouichi
name: Hamaguchi, Kenji
name: Hatsukade, Isamu
name: Hayashi, Katsuhiro
name: Hayashi, Takayuki
name: Hell, Natalie
name: Hodges-Kluck, Edmund
name: Hornschemeier, Ann
name: Ichinohe, Yuto
name: Ishida, Manabu
name: Ishikawa, Kumi
name: Ishisaki, Yoshitaka
name: Kaastra, Jelle
name: Kallman, Timothy
name: Kara, Erin
name: Katsuda, Satoru
name: Kanemaru, Yoshiaki
name: Kelley, Richard
name: Kilbourne, Caroline
name: Kitamoto, Shunji
name: Kobayashi, Shogo
name: Kohmura, Takayoshi
name: Kubota, Aya
name: Leutenegger, Maurice
name: Loewenstein, Michael
name: Maeda, Yoshitomo
name: Markevitch, Maxim
name: Matsumoto, Hironori
name: Matsushita, Kyoko
name: McCammon, Dan
name: McNamara, Brian
name: Mernier, Fran�Ois
name: Miller, Eric D.
name: Miller, Jon M.
name: Mitsuishi, Ikuyuki
name: Mizumoto, Misaki
name: Mizuno, Tsunefumi
name: Mori, Koji
name: Mukai, Koji
name: Murakami, Hiroshi
name: Mushotzky, Richard
name: Nakajima, Hiroshi
name: Nakazawa, Kazuhiro
name: Ness, Jan-Uwe
name: Nobukawa, Kumiko
name: Nobukawa, Masayoshi
name: Noda, Hirofumi
name: Odaka, Hirokazu
name: Ogawa, Shoji
name: Ogorzalek, Anna
name: Okajima, Takashi
name: Ota, Naomi
name: Paltani, Stephane
name: Petre, Robert
name: Plucinsky, Paul
name: Porter, Frederick Scott
name: Pottschmidt, Katja
name: Sato, Kosuke
name: Sato, Toshiki
name: Sawada, Makoto
name: Seta, Hiromi
name: Shidatsu, Megumi
name: Simionescu, Aurora
name: Smith, Randall
name: Suzuki, Hiromasa
name: Szymkowiak, Andrew
name: Takahashi, Hiromitsu
name: Takeo, Mai
name: Tamagawa, Toru
name: Tamura, Keisuke
name: Tanaka, Takaaki
name: Tanimoto, Atsushi
name: Tashiro, Makoto
name: Terada, Yukikatsu
name: Terashima, Yuichi
name: Trigo, Mar�A D�Az
name: Tsuboi, Yohko
name: Tsujimoto, Masahiro
name: Tsunemi, Hiroshi
name: Tsuru, Takeshi G.
name: Uchida, Hiroyuki
name: Uchida, Nagomi
name: Uchida, Yuusuke
name: Uchiyama, Hideki
name: Ueda, Yoshihiro
name: Uno, Shinichiro
name: Vink, Jacco
name: Watanabe, Shin
name: Williams, Brian J.
name: Yamada, Satoshi
name: Yamada, Shinya
name: Yamaguchi, Hiroya
name: Yamaoka, Kazutaka
name: Yamasaki, Noriko Y.
name: Yamauchi, Makoto
name: Yamauchi, Shigeo
name: Yaqoob, Tahir
name: Yoneyama, Tomokage
name: Yoshida, Tessei
name: Yukita, Mihoko
name: Zhuravleva, Irina
name: Kondo, Marie
name: Werner, Norbert
name: Pl?Ek, Tom�?
name: Sun, Ming
name: Hosogi, Kokoro
name: Majumder, Anwesh
name: XRISM Collaboration
Publisher: name: Nature
Year: 2025
Subjects: subject: High-energy astrophysics
subject: Galaxies and clusters

description: Galaxy clusters contain vast amounts of hot ionized gas known as the intracluster medium (ICM). In relaxed cluster cores, the radiative cooling time of the ICM is shorter than the age of the cluster. However, the absence of line emission associated with cooling suggests heating mechanisms that offset the cooling, with feedback from active galactic nuclei (AGNs) being the most likely source1,2. Turbulence and bulk motions, such as the oscillating (?sloshing?) motion of the core gas in the cluster potential well, have also been proposed as mechanisms for heat distribution from the outside of the core3,4. Here we present X-ray spectroscopic observations of the Centaurus galaxy cluster with the X-Ray Imaging and Spectroscopy Mission satellite. We find that the hot gas flows along the line of sight relative to the central galaxy, with velocities from 130?km?s?1 to 310?km?s?1 within about�30?kpc of the centre. This indicates bulk flow consistent with core gas sloshing. Although the bulk flow may prevent excessive accumulation of cooled gas at the centre, it could distribute the heat injected by the AGN and bring in thermal energy from the surrounding ICM. The velocity dispersion of the gas is found to be only ?120?km?s?1 in the core, even within about 10?kpc of the AGN. This suggests that the influence of the AGN on the surrounding ICM motion is limited in the cluster.