Flybys, orbits, splashback: subhalos and the importance of the halo boundary

TL;DR

This paper investigates how different definitions of halo boundaries, especially the splashback radius, affect the classification and abundance of subhalos and flyby halos, revealing significant implications for structure formation models.

Contribution

It systematically quantifies the impact of various halo boundary definitions on subhalo and flyby halo classifications, introducing a universal function for subhalo fraction.

Findings

Splashback radius can double subhalo abundance compared to virial radius.

Subhalo fraction depends strongly on the boundary definition and can vary by factors of two.

A universal function relates subhalo fraction to peak height and power spectrum slope.

Abstract

The classification of dark matter halos as isolated hosts or subhalos is critical for our understanding of structure formation and the galaxy-halo connection. Most commonly, subhalos are defined to reside inside a spherical overdensity boundary such as the virial radius. The resulting host-subhalo relations depend sensitively on the somewhat arbitrary overdensity threshold, but the impact of this dependence is rarely quantified. The recently proposed splashback radius tends to be larger and to include more subhalos than even the largest spherical overdensity boundaries. We systematically investigate the dependence of the subhalo fraction on the radius definition and show that it can vary by factors of unity between different spherical overdensity definitions. Using splashback radii can yet double the abundance of subhalos compared to the virial definition. We also quantify the abundance of flyby (or backsplash) halos, hosts that used to be subhalos in the past. We show that the majority of these objects are mislabeled satellites that are naturally classified as subhalos when we use the splashback radius. We show that the subhalo fraction can be understood as a universal function of only peak height and the slope of the linear power spectrum. We provide a simple fitting function that captures our simulation results to 20% accuracy across a wide range of halo masses, redshifts, and cosmologies. Finally, we demonstrate that splashback radii significantly change our understanding of satellite and flyby galaxies in the Local Group.