Abstract
The Planck Collaboration has shown that the number of clusters as a function of their mass and redshift is an extremely powerful tool for cosmological analyses. However, the true cluster mass is not directly measurable. Among the possible approaches, clusters mass could be related to different observables via self similar scaling law. These observables are related to the baryonic components of which a cluster is composed. However, the theoretical relations that allow the use of these proxies often are affected by observational and physical biases, which impacts on the determination of the cluster mass. Fortunately, cosmological simulations are an extremely powerful tool to assess these problems. We present our calibration of the scaling relation between mass and velocity dispersion of galaxy members from the study of the simulated clusters of The Three Hundred project with mass above 1013M⊙. In order to investigate the presence of a redshift dependence, we analyzed 16 different redshifts between z = 0 and z = 2. Finally, we investigated the impact of different AGN feedback models.
Highlights
According to the hierarchical bottom-up scenario, galaxy clusters (GC) are the last structure to form, and are, the perfect tracers of the evolution of structures along the history of the Universe. They reside in the deepest potential wells of the Large Scale Structure (LSS), generate by accretion of Dark matter (DM) [1], their number as a function of their mass is very sensitive to the underlying Cosmology [2]
In this work we presented the calibration of a scaling relation between the velocity dispersion and the mass of GCs
For this purpose we used the synthetic clusters from the The300 simulation with mass M200 ≥ 1013M, at 16 different redshifts between z = 0 and z = 2, from two different runs, Gadget-X and GIZMO-SIMBA
Summary
According to the hierarchical bottom-up scenario, galaxy clusters (GC) are the last structure to form, and are, the perfect tracers of the evolution of structures along the history of the Universe They reside in the deepest potential wells of the Large Scale Structure (LSS), generate by accretion of Dark matter (DM) [1], their number as a function of their mass is very sensitive to the underlying Cosmology [2]. Since GC formation is gravitationaly driven starting from initial density fluctuations, they evolve self- [3] and this allow us to approximate these scaling relation to power laws This property has been shown to be fundamental for the use of clusters in cosmology, as their mass is not directly measurable.
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