Velocity dispersion of brightest cluster galaxies in cosmological simulations
| Autor: | I. Marini, C. Ragone-Figueroa, Giuseppe Murante, A. Saro, Barbara Sartoris, A Ragagnin, Gian Luigi Granato, Klaus Dolag, Stefano Borgani, Yang Wang |
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| Přispěvatelé: | Marini, I, Borgani, S, Saro, A, Granato, Gl, Ragone-Figueroa, C, Sartoris, B, Dolag, K, Murante, G, Ragagnin, A, Wang, Y |
| Jazyk: | angličtina |
| Rok vydání: | 2021 |
| Předmět: |
Cosmology and Nongalactic Astrophysics (astro-ph.CO)
Stellar mass Star (game theory) Dark matter FOS: Physical sciences Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics 010303 astronomy & astrophysics Galaxy cluster Astrophysics::Galaxy Astrophysics Physics 010308 nuclear & particles physics galaxies clusters general Velocity dispersion Astronomy and Astrophysics Astrophysics - Astrophysics of Galaxies Galaxy Redshift methods numerical galaxies elliptical and lenticular cD galaxies evolution galaxies stellar content Stars Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) Astrophysics::Earth and Planetary Astrophysics Astrophysics - Cosmology and Nongalactic Astrophysics |
| Popis: | Using the DIANOGA hydrodynamical zoom-in simulation set of galaxy clusters, we analyze the dynamics traced by stars belonging to the Brightest Cluster Galaxies (BCGs) and their surrounding diffuse component, forming the intracluster light (ICL), and compare it to the dynamics traced by dark matter and galaxies identified in the simulations. We compute scaling relations between 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 good agreement with observational results. Our simulations also predict $\sigma_\mathrm{BCG}^{\star}$- $\sigma_{200}$ relation to not change significantly up to redshift $z=1$, in line with a relatively slow accretion of the BCG stellar mass at late times. We analyze the main features of the velocity dispersion profiles, as traced by stars, dark matter, and galaxies. As a result, we discuss that observed stellar velocity dispersion profiles in the inner cluster regions are in excellent agreement with simulations. We also report that the slopes of the BCG velocity dispersion profile from simulations agree with what is measured in observations, confirming the existence of a robust correlation between the stellar velocity dispersion slope and the cluster velocity dispersion (thus, cluster mass) when the former is computed within $0.1 R_{500}$. Our results demonstrate that simulations can correctly describe the dynamics of BCGs and their surrounding stellar envelope, as determined by the past star-formation and assembly histories of the most massive galaxies of the Universe. Comment: 16 pages, 14 figures |
| Databáze: | OpenAIRE |
| Externí odkaz: |
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