Angelinelli, M.M.AngelinelliETTORI, STEFANOSTEFANOETTORIDolag, K.K.DolagVAZZA, FrancoFrancoVAZZARAGAGNIN, AntonioAntonioRAGAGNIN2025-01-102025-01-1020220004-6361http://hdl.handle.net/20.500.12386/35623We study the distributions of the baryons in massive halos ($M_{vir} > 10^{13} \ h^{-1}M_{\odot}$) in the $Magneticum$ suite of Smoothed Particle Hydrodynamical cosmological simulations, out to the unprecedented radial extent of $10 R_{500,\mathrm c}$. We confirm that, under the action of non-gravitational physical phenomena, the baryon mass fraction is lower in the inner regions ($<R_{500,\mathrm c}$) of increasingly less massive halos, and rises moving outwards, with values that spans from 51% (87%) in the regions around $R_{500,\mathrm c}$ to 95% (100%) at $10R_{500,\mathrm c}$ of the cosmological value in the systems with the lowest (highest; $M_{vir} \sim 5 \times 10^{14} \ h^{-1}M_{\odot}$) masses. The galaxy groups almost match the gas (and baryon) fraction measured in the most massive halos only at very large radii ($r>6 R_{500,\mathrm c}$), where the baryon depletion factor $Y_{\rm bar} = f_{\rm bar} / (\Omega_{\rm b}/\Omega_{\rm m})$ approaches the value of unity, expected for "closed-box" systems. We find that both the radial and mass dependency of the baryon, gas, and hot depletion factors are predictable and follow a simple functional form. The star mass fraction is higher in less massive systems, decreases systematically with increasing radii, and reaches a constant value of $Y_{\rm star} \approx 0.09$, where also the gas metallicity is constant, regardless of the host halo mass, as a result of the early ($z>2$) enrichment process.STAMPAenArticle10.1051/0004-6361/2022440682-s2.0-85134880809https://www.aanda.org/articles/aa/full_html/2022/07/aa44068-22/aa44068-22.htmlhttp://arxiv.org/abs/2206.08382v1FIS/05 - ASTRONOMIA E ASTROFISICA