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

被引:23
作者
Angelinelli, M. [1 ,2 ]
Ettori, S. [2 ,3 ]
Dolag, K. [4 ,5 ]
Vazza, F. [1 ,6 ,7 ]
Ragagnin, A. [1 ,8 ,9 ]
机构
[1] Univ Bologna, Dipartimento Fis & Astron, Via Gobetti 92-3, I-40121 Bologna, Italy
[2] Osservatorio Astrofis & Sci Spazio, INAF, Via Pietro Gobetti 93-3, I-40121 Bologna, Italy
[3] Ist Nazl Fis Nucl, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy
[4] Univ Sternwarte, Ludwig Maximilians Univ Munchen, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany
[5] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany
[6] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany
[7] INAF, Ist Radio Astron, Via Gobetti 101, I-40121 Bologna, Italy
[8] Osserv Astron Trieste, INAF, Via GB Tiepolo 11, I-34143 Trieste, Italy
[9] Inst Fundamental Phys Universe, IFPU, Via Beirut 2, I-34014 Trieste, Italy
基金
欧洲研究理事会; 欧盟地平线“2020”;
关键词
methods: numerical; large-scale structure of Universe; galaxies: clusters: intracluster medium; galaxies: groups: general; hydrodynamics; galaxies: clusters: general; ACTIVE GALACTIC NUCLEI; PARTICLE HYDRODYNAMICS SIMULATIONS; X-RAY OBSERVATIONS; GALAXY CLUSTERS; INTRACLUSTER MEDIUM; COSMOLOGICAL SIMULATION; GAS MOTIONS; ENRICHMENT; EVOLUTION; FEEDBACK;
D O I
10.1051/0004-6361/202244068
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We study the distributions of the baryons in massive halos (M-vir > 10(13) h(-1) M-circle dot) 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,R-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,R-c to 95% (100%) at 10R(500,c) in the systems with the lowest (highest; M-vir similar to 5 x 10(14) h(-1) M-circle dot) 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)/(Omega(b)/Omega(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 approximate to 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.
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页数:8
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