Velocity dispersion vs cluster mass: a new scaling law with The Three Hundred clusters

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 \THP{} project with mass above $10^{13}{M}_{\odot }$. 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.

To appear in the Proceedings of the International Conference entitled "mm Universe @ NIKA2", Rome (Italy), June 2021, EPJ Web of conferences

References in corpus (3)

• Simba: Cosmological Simulations with Black Hole Growth and Feedback
• Virial Scaling of Massive Dark Matter Halos: Why Clusters Prefer a High Normalization Cosmology
• The relation between velocity dispersion and mass in simulated clusters of galaxies: dependence on the tracer and the baryonic physics

Cited by in corpus (6)

• \textsc{The Three Hundred} project: The \textsc{Gizmo-Simba} run
• The massive relic galaxy NGC 1277 is dark matter deficient. From dynamical models of integral-field stellar kinematics out to five effective radii
• Characterising the intra-cluster light in The Three Hundred simulations
• What to expect from dynamical modelling of cluster haloes II. Investigating dynamical state indicators with Random Forest
• FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
• Modelling the selection of galaxy groups with end to end simulations