On the redshift evolution of the baryon and gas fraction in simulated groups and clusters of galaxies

Abstract

We study the redshift evolution of the baryon budget in a large set of galaxy clusters from the {\it Magneticum} suite of SPH cosmological simulations. At high redshifts, we obtain "closed box" systems independently by the mass of the systems on radii greater than $3R_{500,\mathrm{c}}$, whereas at lower redshifts, only the most massive halos could be considered as `"closed box". The baryon fraction shows a general decrease with the redshift and, for less massive objects, we observe a much more prominent decrease than for massive halos. The gas depletion parameter $Y_{\mathrm{gas}}$ shows a steeper and highly scattered radial distribution in the central regions of less massive halos with respect to massive objects at all redshifts, while on larger radii the gas fraction distributions are independent of the masses or the redshifts. The hot component of the gas traces well the total amount of gas at low redshifts. At higher redshifts, the cold component provides a not negligible contribution to the total amount of baryon in our systems. Moreover, the behaviour of the baryonic, entire gas, and hot gas phase depletion parameters as a function of radius, mass, and redshift are described by some functional forms. The evolution of metallicity and stellar mass in halos suggests that the early enrichment process is dominant. We investigate correlations between the time evolution of AGN feedback and the depletion parameters. We demonstrate that the energy injected by the AGN activity shows a particularly strong positive correlation with $Y_{\mathrm{bar}}$, $Y_{\mathrm{cold}}$,$Y_{\mathrm{star}}$ and a negative one with $Y_{\mathrm{hot}}$, $Z_{\mathrm{Tot}}$. These trends are consistent with previous works, meaning that our results, combined with findings derived from current and future X-rays observations, represent possible proxies to test the AGN feedback models used in different suites of numerical simulations.

Accepted in A&A, 15 pages, 11 figures

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• Detecting clusters and groups of galaxies populating the local Universe in large optical spectroscopic surveys
• Halo Scaling Relations and Hydrostatic Mass Bias in the Simba Simulation From Realistic Mock X-ray Catalogues
• The impact of assembly history on the X-ray detectability of halos. From galaxy groups to galaxy clusters
• How the cool-core population transitions from galaxy groups to massive clusters: A comparison of the largest Magneticum simulation with eROSITA, XMM-Newton, Chandra and LOFAR observations
• The Three Hundred Project: Modeling Baryon and Hot-Gas Fraction Evolution in Simulated Clusters
• A full reconstruction of two galaxy clusters intra-cluster medium with strong gravitational lensing
• Comparison of $\Lambda$CDM and $R_h=ct$ with updated galaxy cluster $f_{gas}$ measurements using Bayesian inference
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