The Case for Hot-Mode Accretion in Abell 2029

Deovrat Prasad; G. Mark Voit; Brian W. O'Shea

doi:10.1093/mnras/stae1203

paper

The Case for Hot-Mode Accretion in Abell 2029

arXiv:2311.05704 · doi:10.1093/mnras/stae1203

Abstract

Radiative cooling and AGN heating are thought to form a feedback loop that regulates the evolution of low redshift cool-core galaxy clusters. Numerical simulations suggest that formation of multiphase gas in the cluster core imposes a floor on the ratio of cooling time ( $t_{cool}$ ) to free-fall time ( $t_{ff}$ ) at $min (t_{cool} / t_{ff}) \approx 10$ . Observations of galaxy clusters show evidence for such a floor, and usually the cluster cores with $min (t_{cool} / t_{ff}) ≲ 30$ contain abundant multiphase gas. However, there are important outliers. One of them is Abell 2029, a massive galaxy cluster ( $M_{200} ≳ 1 0^{15}$ M $_{⊙}$ ) with $min (t_{cool} / t_{ff}) \sim 20$ , but little apparent multiphase gas. In this paper, we present high resolution 3D hydrodynamic AMR simulations of a cluster similar to A2029 and study how it evolves over a period of 1-2 Gyr. Those simulations suggest that Abell 2029 self-regulates without producing multiphase gas because the mass of its central black hole ( $\sim 5 \times 1 0^{10} M_{⊙}$ ) is great enough for Bondi accretion of hot ambient gas to produce enough feedback energy to compensate for radiative cooling.

8 pages, 5 figures, Published in MNRAS

The Case for Hot-Mode Accretion in Abell 2029

Abstract

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