Exploring the role of cosmological shock waves in the Dianoga simulations of galaxy clusters

Author:

Planelles S12,Borgani S3456,Quilis V12ORCID,Murante G36ORCID,Biffi V67ORCID,Rasia E36,Dolag K78,Granato G L369ORCID,Ragone-Figueroa C39

Affiliation:

1. Departament d’Astronomia i Astrofísica, Universitat de València, c/ Dr. Moliner, 50, E-46100, Burjassot (Valencia), Spain

2. Observatori Astronòmic, Universitat de València, E-46980 Paterna (Valencia), Spain

3. INAF, Osservatorio Astronomico di Trieste, via Tiepolo 11, I-34131, Trieste, Italy

4. Dipartimento di Fisica dell’ Università di Trieste, Sezione di Astronomia, via Tiepolo 11, I-34131 Trieste, Italy

5. INFN, Instituto Nazionale di Fisica Nucleare, Via Valerio 2, I-34127, Trieste, Italy

6. IFPU, Institute for Fundamental Physics of the Universe, Via Beirut 2, I-34014 Trieste, Italy

7. University Observatory Munich, Scheinerstr. 1, D-81679 Munich, Germany

8. Max-Planck-Institut für Astrophysik, Karl-Schwarzschild Strasse 1, D-85748 Garching bei München, Germany

9. Instituto de Astronomía Teórica y Experimental (IATE), Consejo Nacional de Investigaciones Científicas y Técnicas de la, República Argentina (CONICET) Universidad Nacional de Córdoba, Laprida 854, X5000BGR, Córdoba, Argentina

Abstract

ABSTRACT Cosmological shock waves are ubiquitous to cosmic structure formation and evolution. As a consequence, they play a major role in the energy distribution and thermalization of the intergalactic medium (IGM). We analyze the Mach number distribution in the Dianoga simulations of galaxy clusters performed with the SPH code gadget-3. The simulations include the effects of radiative cooling, star formation, metal enrichment, supernova, and active galactic nuclei feedback. A grid-based shock-finding algorithm is applied in post-processing to the outputs of the simulations. This procedure allows us to explore in detail the distribution of shocked cells and their strengths as a function of cluster mass, redshift, and baryonic physics. We also pay special attention to the connection between shock waves and the cool-core/non-cool-core (CC/NCC) state and the global dynamical status of the simulated clusters. In terms of general shock statistics, we obtain a broad agreement with previous works, with weak (low-Mach number) shocks filling most of the volume and processing most of the total thermal energy flux. As a function of cluster mass, we find that massive clusters seem more efficient in thermalizing the IGM and tend to show larger external accretion shocks than less massive systems. We do not find any relevant difference between CC and NCC clusters. However, we find a mild dependence of the radial distribution of the shock Mach number on the cluster dynamical state, with disturbed systems showing stronger shocks than regular ones throughout the cluster volume.

Funder

Università degli Studi di Trieste

MICINN

Generalitat Valenciana

MIUR

INFN

DFG

Deutsche Forschungsgemeinschaft

European Research Council

Horizon 2020

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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