Abstract
ABSTRACT Using the catalogues of galaxy clusters from The Three Hundred project, modelled with both hydrodynamic simulations (gadget-x and gadget-music), and semi-analytical models (SAMs), we study the scatter and self-similarity of the profiles and distributions of the baryonic components of the clusters: the stellar and gas mass, metallicity, the stellar age, gas temperature, and the (specific) star formation rate. Through comparisons with observational results, we find that the shape and the scatter of the gas density profiles matches well the observed trends including the reduced scatter at large radii which is a signature of self-similarity suggested in previous studies. One of our simulated sets, gadget-x, reproduces well the shape of the observed temperature profile, while gadget-music has a higher and flatter profile in the cluster centre and a lower and steeper profile at large radii. The gas metallicity profiles from both simulation sets, despite following the observed trend, have a relatively lower normalization. The cumulative stellar density profiles from SAMs are in better agreement with the observed result than both hydrodynamic simulations which show relatively higher profiles. The scatter in these physical profiles, especially in the cluster centre region, shows a dependence on the cluster dynamical state and on the cool-core/non-cool-core dichotomy. The stellar age, metallicity, and (s)SFR show very large scatter, which are then presented in 2D maps. We also do not find any clear radial dependence of these properties. However, the brightest central galaxies have distinguishable features compared to the properties of the satellite galaxies.
Highlights
Galaxy clusters are the largest gravitationally bound objects in the universe, containing numerous galaxies, intracluster medium (ICM), and dark matter
For the stellar physical profiles, we focus on stellar density, age, and metallicity, which are all derived only from the satellite galaxies
For the gaseous physical profiles, we investigate the gas density, temperature, metallicity, star formation rate (SFR), and specific star formation rate (sSFR) properties, which are based only on the gas content from the two hydrodynamical runs
Summary
Galaxy clusters are the largest gravitationally bound objects in the universe, containing numerous galaxies, intracluster medium (ICM), and dark matter. An open question is whether the gas/stars and their physical property profiles, such as temperature, metallicity, follow a similar trend and these profiles are model dependent or not. The gas density profile has been well studied in the outskirts from both numerical and observational studies (Roncarelli et al 2006; Vikhlinin et al 2006; Lemze et al 2008) These works found that the outer radii profile can be fitted by a power law while in the innermost regions the gas density profile is more cored than the dark matter density profile, even though the trend of the core depends on the cluster dynamical status. The gas temperature profile slowly increases from the outer regions towards the cluster centre (e.g. Vikhlinin et al 2005; Pratt et al 2007; Rasmussen & Ponman 2007; Reiprich et al 2009).
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