Velocity dispersion of brightest cluster galaxies in cosmological simulations

Using the DIANOGA hydrodynamical zoom-in simulation set of galaxy clusters, we analyze dynamics traced by stars belonging to Brightest Cluster Galaxies (BCGs) and their surrounding diffuse component, forming intracluster light (ICL), compare it dark matter galaxies identified in simulations. We compute scaling relations between BCG cluster velocity dispersions corresponding masses (i.e. $M_\mathrm{BCG}^{\star}$- $\sigma_\mathrm{BCG}^{\star}$, $M_{200}$- $\sigma_{200}$, $M_{200}$, $\sigma_\mathrm{BCG}^{\star}$- $\sigma_{200}$), find general a good agreement with observational results. Our simulations also predict $\sigma_{200}$ relation not change significantly up redshift $z=1$, line relatively slow accretion stellar mass at late times. main features dispersion profiles, as stars, matter, galaxies. As result, discuss that observed profiles inner regions are excellent report slopes profile from agree what is measured observations, confirming existence robust correlation slope (thus, mass) when former computed within $0.1 R_{500}$. results demonstrate can correctly describe BCGs envelope, determined past star-formation assembly histories most massive Universe.