Germany\
    $^{9}$ INFN, Instituto Nazionale di Fisica Nucleare, Trieste, Italy\
    $^{10}$ Instituto di Astronomía Teórica y Experimental (IATE), Consejo Nacional de Investigaciones Científicas y Técnicas de la República Argentina (CONICET),\
         Observatorio Astronómico, Universidad Nacional de Córboda, Laprida 854, X50000BGR, Córdoba, Argentina
bibliography:
- 'ref.bib'
title: 'Hydrodynamic Simulations of Galaxy Clusters: Scaling Relations and Evolution'
---

[galaxies: clusters: general — galaxies: clusters: intracluster medium — X-ray: galaxy: clusters — methods: numerical]{}

Introduction {#sec:intro}
============

Clusters of galaxies are the latest gravitationally bound structures to form. They begin their collapse at around redshift $z \sim 2$ when the dark-energy component starts to be relevant (even if not dominant yet) and just after the baryonic Universe has experienced an extremely energetic phase due to the high star formation level and the intense AGN (Active Galactic Nuclei) activity [@aird.etal.2015]. For the reason that clusters’ formation happens in such peculiar time, these massive objects are an invaluable laboratory for the study of astrophysical processes and for the derivation of cosmological parameters.

High-redshift investigations and the comparison with local observations are particularly advantageous. One of the most powerful cosmological measure is, indeed, the [*evolution*]{} of the mass function [@borgani_guzzo; @voit2005; @2009ApJ...692.1033V; @allen.etal.2011; @2011ASL.....4..204B; @2015SSRv..188...93P]. As other 