A dynamics-based density profile for dark haloes. I. Algorithm and basic results

TL;DR

This paper introduces a new algorithm to analyze dark matter halo density profiles by separating orbiting and infalling matter, revealing how these profiles depend on halo dynamics, accretion rates, and cosmological parameters.

Contribution

The paper presents a novel method to dynamically disentangle orbiting and infalling components in halo profiles using pericentric passage counts, providing new insights into halo structure and evolution.

Findings

Orbiting term sharply truncates at the edge of the orbit distribution.

Profile shape primarily depends on halo dynamics and accretion rate.

Infalling term varies with environment and accretion rate, showing diverse shapes.

Abstract

The density profiles of dark matter haloes can potentially probe dynamics, fundamental physics, and cosmology, but some of the most promising signals reside near or beyond the virial radius. While these scales have recently become observable, the profiles at large radii are still poorly understood theoretically, chiefly because the distribution of orbiting matter (the one-halo term) is partially concealed by particles falling into halos for the first time. We present an algorithm to dynamically disentangle the orbiting and infalling contributions by counting the pericentric passages of billions of simulation particles. We analyse dynamically split profiles out to 10 R200m across a wide range of halo mass, redshift, and cosmology. We show that the orbiting term experiences a sharp truncation at the edge of the orbit distribution. Its sharpness and position are mostly determined by the mass accretion rate, confirming that the entire profile shape primarily depends on halo dynamics and secondarily on mass, redshift, and cosmology. The infalling term also depends on the accretion rate for fast-accreting haloes but is mostly set by the environment for slowly accreting haloes, leading to a diverse array of shapes that does not conform to simple theoretical models. While the resulting scatter in the infalling term reaches 1 dex, the scatter in the orbiting term is only between 0.1 and 0.4 dex and almost independent of radius. We demonstrate a tight correspondence between the redshift evolution in LCDM and the slope of the matter power spectrum. Our code and data are publicly available.