2025Natur.638..365X

Query : 2025Natur.638..365X

2025Natur.638..365X - Nature, 638, 365-369 (2025/February-0)

The bulk motion of gas in the core of the Centaurus galaxy cluster.

XRISM COLLABORATION, AUDARD M., AWAKI H., BALLHAUSEN R., BAMBA A., BEHAR E., BOISSAY-MALAQUIN R., BRENNEMAN L., BROWN G.V., CORRALES L., COSTANTINI E., CUMBEE R., DONE C., DOTANI T., EBISAWA K., ECKART M.E., ECKERT D., ENOTO T., EGUCHI S., EZOE Y., FOSTER A., FUJIMOTO R., FUJITA Y., FUKAZAWA Y., FUKUSHIMA K., FURUZAWA A., GALLO L., GARCIA J.A., GU L., GUAINAZZI M., HAGINO K., HAMAGUCHI K., HATSUKADE I., HAYASHI K., HAYASHI T., HELL N., HODGES-KLUCK E., HORNSCHEMEIER A., ICHINOHE Y., ISHIDA M., ISHIKAWA K., ISHISAKI Y., KAASTRA J., KALLMAN T., KARA E., KATSUDA S., KANEMARU Y., KELLEY R., KILBOURNE C., KITAMOTO S., KOBAYASHI S., KOHMURA T., KUBOTA A., LEUTENEGGER M., LOEWENSTEIN M., MAEDA Y., MARKEVITCH M., MATSUMOTO H., MATSUSHITA K., McCAMMON D., McNAMARA B., MERNIER F., MILLER E.D., MILLER J.M., MITSUISHI I., MIZUMOTO M., MIZUNO T., MORI K., MUKAI K., MURAKAMI H., MUSHOTZKY R., NAKAJIMA H., NAKAZAWA K., NESS J.-U., NOBUKAWA K., NOBUKAWA M., NODA H., ODAKA H., OGAWA S., OGORZALEK A., OKAJIMA T., OTA N., PALTANI S., PETRE R., PLUCINSKY P., PORTER F.S., POTTSCHMIDT K., SATO K., SATO T., SAWADA M., SETA H., SHIDATSU M., SIMIONESCU A., SMITH R., SUZUKI H., SZYMKOWIAK A., TAKAHASHI H., TAKEO M., TAMAGAWA T., TAMURA K., TANAKA T., TANIMOTO A., TASHIRO M., TERADA Y., TERASHIMA Y., DIAZ TRIGO M., TSUBOI Y., TSUJIMOTO M., TSUNEMI H., TSURU T.G., UCHIDA H., UCHIDA N., UCHIDA Y., UCHIYAMA H., UEDA Y., UNO S., VINK J., WATANABE S., WILLIAMS B.J., YAMADA S., YAMADA S., YAMAGUCHI H., YAMAOKA K., YAMASAKI N.Y., YAMAUCHI M., YAMAUCHI S., YAQOOB T., YONEYAMA T., YOSHIDA T., YUKITA M., ZHURAVLEVA I., KONDO M., WERNER N., PLSEK T., SUN M., HOSOGI K. and MAJUMDER A.

Abstract (from CDS):

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 source . 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 core . 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.

Abstract Copyright: 2025 The Author(s), under exclusive licence to Springer Nature Limited

Journal keyword(s):

Simbad objects: 6

Full paper

View the references in ADS

Number of rows : 6

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag B	Mag V	Mag R	Sp type	#ref 1850 - 2026	#notes
1	ACO 426	ClG	03 19 47.6	+41 30 54				~	2508	1
2	ACO 3526	ClG	12 48 49.2	-41 18 17				~	1154	2
3	NGC 4696	rG	12 48 49.2724775784	-41 18 39.304053252	11.21		10.7	~	510	3
4	NAME Cen 30	ClG	12 48 51.7	-41 18 21				~	66	0
5	NAME Cen 45	GrG	12 50	-41.3				~	51	0
6	NGC 4709	Sy2	12 50 03.9037103928	-41 22 55.094298420	12.48	11.32	10.89	~	134	0

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