Simulating the LOcal Web (SLOW) II. Properties of local galaxy clusters

被引：7

作者：

Hernandez-Martinez, Elena ^{[1
]}

Dolag, Klaus ^{[1
,2
]}

Seidel, Benjamin ^{[1
]}

Sorce, Jenny G. ^{[3
,4
,5
]}

Aghanim, Nabila ^{[4
]}

Pilipenko, Sergey ^{[9
]}

Gottloeber, Stefan ^{[5
]}

Lebeau, Theo ^{[4
]}

Valentini, Milena ^{[1
,6
,7
,8
]}

机构：

[1] Ludwig Maximilians Univ Munchen, Univ Sternwarte, Fak Phys, Scheinerstr1, D-81679 Munich, Germany

[2] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany

[3] Univ Lille, CNRS, Cent Lille, UMR 9189,CRIStAL, F-59000 Lille, France

[4] Univ Paris Saclay, Inst Astrophys Spatiale, CNRS, F-91405 Orsay, France

[5] Leibniz Inst Astrophys AIP, Sternwarte 16, D-14482 Potsdam, Germany

[6] Univ Trieste, Dept Phys, Astron Unit, Via Tiepolo 11, I-34131 Trieste, Italy

[7] ICSC Italian Res Ctr High Performance Comp Big Dat, Bologna, Italy

[8] INAF Osservatorio Astron Trieste, Via Tiepolo 11, I-34131 Trieste, Italy

[9] Russian Acad Sci, PN Lebedev Phys Inst, Profsojuznaja St 84-32, Moscow 117997, Russia

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 687卷

基金：

欧洲研究理事会;

关键词：

methods: numerical; galaxies: clusters: general; large-scale structure of Universe; COSMOLOGICAL INITIAL CONDITIONS; PARTICLE HYDRODYNAMICS SIMULATIONS; ACTIVE GALACTIC NUCLEI; X-RAY MORPHOLOGY; VIRGO CLUSTER; DARK-MATTER; SCALING RELATIONS; COMA CLUSTER; PECULIAR VELOCITIES; REDSHIFT EVOLUTION;

D O I：

10.1051/0004-6361/202449460

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. This is the second paper in a series presenting the results from a 500 h(-1) Mpc large constrained simulation of the local Universe (SLOW). The initial conditions for this cosmological hydro-dynamical simulation are based on peculiar velocities derived from the CosmicFlows-2 catalog. The simulation follows cooling, star formation, and the evolution of super-massive black holes. This allows one to directly predict observable properties of the intracluster medium (ICM) within galaxy clusters, including X-ray luminosity, temperatures, and the Compton-y signal. Aims. Comparing the properties of observed galaxy clusters within the local Universe with the properties of their simulated counterparts enables us to assess the effectiveness of the initial condition constraints in accurately replicating the mildly nonlinear properties of the largest, collapsed objects within the simulation. Methods. Based on the combination of several, publicly available surveys we compiled a sample of galaxy clusters within the local Universe, of which we were able to cross-identify 46 of them with an associated counterpart within the SLOW simulation. We then derived the probability of the cross identification based on mass, X-ray luminosity, temperature, and Compton-y by comparing it to a random selection. Results. Our set of 46 cross-identified local Universe clusters contains the 13 most massive clusters from the Planck SZ catalog as well as 70% of clusters with M-500 larger than 2 x 10(14) M-circle dot. Compared to previous constrained simulations of the local volume, we found in SLOW a much larger amount of replicated galaxy clusters, where their simulation-based mass prediction falls within the uncertainties of the observational mass estimates. Comparing the median observed and simulated masses of our cross-identified sample allows us to independently deduce a hydrostatic mass bias of (1 - b)approximate to 0.87. Conclusions. The SLOW constrained simulation of the local Universe faithfully reproduces numerous fundamental characteristics of a sizable number of galaxy clusters within our local neighborhood, opening a new avenue for studying the formation and evolution of a large set of individual galaxy clusters as well as testing our understanding of physical processes governing the ICM.

引用

页数：19

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