Mapping `out-of-the-box' the properties of the baryons in massive halos

We study the distributions of the baryons in massive halos (M_vir > 10¹³ h⁻¹ M_⊙) in the Magneticum suite of smoothed particle hydrodynamical cosmological simulations, out to the unprecedented radial extent of 10R_{500, c}. We confirm that, under the action of non-gravitational physical phenomena, the baryon mass fraction is lower in the inner regions (< R_{500, c}) of increasingly less massive halos, and rises moving outwards, with values that span from 51% (87%) of the cosmological value in the regions around R_{500, c} to 95% (100%) at 10R_{500, c} in the systems with the lowest (highest; M_vir ∼ 5 × 10¹⁴ h⁻¹ M_⊙) masses. The galaxy groups almost match the gas (and baryon) fraction measured in the most massive halos only at very large radii (r > 6R_{500, c}), where the baryon depletion factor Y_bar = f_bar/(Ω_b/Ω_m) approaches the value of unity, expected for `closed-box' systems. We find that both the radial and mass dependence 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_star ≈ 0.09, where the gas metallicity is also constant, regardless of the host halo mass, as a result of the early (z > 2) enrichment process.