Accurate Model of the Projected Velocity Distribution of Galaxies in Dark Matter Halos

Abstract

We present a percent-level accurate model of the line-of-sight velocity distribution of galaxies around dark matter halos as a function of projected radius and halo mass. The model is developed and tested using synthetic galaxy catalogs generated with the UniverseMachine run on the Multi-Dark Planck 2 N-body simulations. The model decomposes the galaxies around a cluster into three kinematically distinct classes: orbiting, infalling, and interloping galaxies. We demonstrate that: 1) we can statistically distinguish between these three types of galaxies using only projected line-of-sight velocity information; 2) the halo edge radius inferred from the line-of-sight velocity dispersion is an excellent proxy for the three-dimensional halo edge radius; 3) we can accurately recover the full velocity dispersion profile for each of the three populations of galaxies. Importantly, the velocity dispersion profiles of the orbiting and infalling galaxies contain five independent parameters -- three distinct radial scales and two velocity dispersion amplitudes -- each of which is correlated with mass. Thus, the velocity dispersion profile of galaxy clusters has inherent redundancies that allow us to perform nontrivial systematics check from a single data set. We discuss several potential applications of our new model for detecting the edge radius and constraining cosmology and astrophysics using upcoming spectroscopic surveys.

arXiv comment10 pages, 11 figures, accepted in MNRAS

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• C2-GaMe: Classification of Cluster Galaxy Membership with Machine Learning
• A full reconstruction of two galaxy clusters intra-cluster medium with strong gravitational lensing
• Perseus cluster in its X-ray entirety with SRG/eROSITA. Merger and Radio-Uroboroses