Observing dynamical friction in galaxy clusters

Abstract

We present a novel method to detect the effects of dynamical friction in observed galaxy clusters. Following accretion into clusters, massive satellite galaxies will backsplash to systematically smaller radii than less massive satellites, an effect that may be detected by stacking the number density profiles of galaxies around clusters. We show that this effect may be understood using a simple toy model which reproduces the trends with halo properties observed in simulations. We search for this effect using SDSS redMaPPer clusters with richness 10<lambda<20, and find that bright (M_i<-21.5) satellites have smaller splashback radii than fainter (M_i>-20) satellites at 99% confidence.

arXiv comment6 pages, to be submitted to JCAP

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Cited by in corpus (37)

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• The Halo Boundary of Galaxy Clusters in the SDSS
• The Splashback Feature around DES Galaxy Clusters: Galaxy Density and Weak Lensing Profiles
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• Lensing Constraints on the Mass Profile Shape and the Splashback Radius of Galaxy Clusters
• Signatures of Self-Interacting dark matter on cluster density profile and subhalo distributions
• The Splashback Radius of Planck-SZ clusters
• The splashback boundary of haloes in hydrodynamic simulations
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• How Accurately Can We Detect the Splashback Radius of Dark Matter Halos and its Correlation With Accretion Rate?
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• Stellar splashback: the edge of the intracluster light
• The Phase Space Structure of Dark Matter Halos
• Tests of Gravity with Galaxy Clusters
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