Splashback in accreting dark matter halos

Abstract

Recent work has shown that density profiles in the outskirts of dark matter halos can become extremely steep over a narrow range of radius. This behavior is produced by splashback material on its first apocentric passage after accretion. We show that the location of this splashback feature may be understood quite simply, from first principles. We present a simple model, based on spherical collapse, that accurately predicts the location of splashback without any free parameters. The important quantities that determine the splashback radius are accretion rate and redshift.

8 pages

References in corpus (6)

• Rotation-Dependent Catastrophic Disruption of Gravitational Aggregates
• The pseudo-evolution of halo mass
• The Unorthodox Orbits of Substructure Halos
• Self-Similar Solutions of Triaxial Dark Matter Halos
• Infall caustics in dark matter halos?
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Cited by in corpus (11)

• Mass Accretion and its Effects on the Self-Similarity of Gas Profiles in the Outskirts of Galaxy Clusters
• The Three Hundred Project: Backsplash galaxies in simulations of clusters
• Lensing Constraints on the Mass Profile Shape and the Splashback Radius of Galaxy Clusters
• A New Method to Quantify Environment and Model Ram-Pressure Stripping in N-Body Simulations
• Tests of Gravity with Galaxy Clusters
• Evolution and Statistics of Non-Sphericity of Dark Matter Halos from Cosmological N-Body Simulation
• Phase-space structure of cold dark matter halos inside splashback: multi-stream flows and self-similar solution
• A Simple Physical Model for the Gas Distribution in Galaxy Clusters
• A Spectroscopic Survey of the Fields of 28 Strong Gravitational Lenses: Implications for $H_0$
• Haloes at the ragged edge: The importance of the splashback radius
• Halo Concentrations and the Fundamental Plane of Galaxy Clusters