English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

Using the DIANOGA hydrodynamical zoom-in simulation set of galaxy clusters,we analyze the dynamics traced by stars belonging to the Brightest ClusterGalaxies (BCGs) and their surrounding diffuse component, forming theintracluster light (ICL), and compare it to the dynamics traced by dark matterand galaxies identified in the simulations. We compute scaling relationsbetween the BCG and cluster velocity dispersions and their corresponding masses(i.e. $M_\mathrm{BCG}^{\star}$- $\sigma_\mathrm{BCG}^{\star}$, $M_{200}$-$\sigma_{200}$, $M_\mathrm{BCG}^{\star}$- $M_{200}$,$\sigma_\mathrm{BCG}^{\star}$- $\sigma_{200}$), we find in general a goodagreement with observational results. Our simulations also predict$\sigma_\mathrm{BCG}^{\star}$- $\sigma_{200}$ relation to not changesignificantly up to redshift $z=1$, in line with a relatively slow accretion ofthe BCG stellar mass at late times. We analyze the main features of thevelocity dispersion profiles, as traced by stars, dark matter, and galaxies. Asa result, we discuss that observed stellar velocity dispersion profiles in theinner cluster regions are in excellent agreement with simulations. We alsoreport that the slopes of the BCG velocity dispersion profile from simulationsagree with what is measured in observations, confirming the existence of arobust correlation between the stellar velocity dispersion slope and thecluster velocity dispersion (thus, cluster mass) when the former is computedwithin $0.1 R_{500}$. Our results demonstrate that simulations can correctlydescribe the dynamics of BCGs and their surrounding stellar envelope, asdetermined by the past star-formation and assembly histories of the mostmassive galaxies of the Universe.

Velocity dispersion of the brightest cluster galaxies in cosmological simulations