The bulk motion of gas in the core of the Centaurus galaxy cluster
| Autoři | |
|---|---|
| Rok publikování | 2025 |
| Druh | Článek v odborném periodiku |
| Časopis / Zdroj | Nature |
| Fakulta / Pracoviště MU | |
| Citace | |
| www | |
| Doi | https://doi.org/10.1038/s41586-024-08561-z |
| Klíčová slova | Galaxies and clusters; High-energy astrophysics |
| Popis | 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(1,2). 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 core(3,4). 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 130kms(-1) to 310kms(-1) within about 30kpc 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 less than or similar to 120kms(-1) in the core, even within about 10kpc of the AGN. This suggests that the influence of the AGN on the surrounding ICM motion is limited in the cluster. |
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