What Do Dark Matter Properties Tell Us About Their Mass Assembly Histories?

TL;DR

This paper investigates how the structural properties of dark matter halos relate to their mass assembly histories, revealing correlations with formation time and growth patterns, and exploring implications for galaxy cluster evolution.

Contribution

It introduces a detailed analysis linking halo structural parameters to their mass accretion histories using principal component analysis, highlighting the roles of early and late formation phases.

Findings

Concentration correlates with early halo history.

Relaxation correlates with late halo history.

Principal components explain about 70% of the scatter in mass accretion histories.

Abstract

Individual dark matter halos in cosmological simulations vary widely in their detailed structural properties such as shape, rotation, substructure and degree of internal relaxation. Recent non-parametric (principal component) analyses suggest that a few principal components explain a large fraction of the scatter in halo properties. The main principal component is closely linked with concentration, which in turn is known to be related to the mass accretion history of the halo. Here we examine more generally the connection between mass accretion history and structural parameters. The space of mass accretion histories has principal components of its own. We find that the strongest two can be interpreted as the overall age of the halo and the acceleration or deceleration of growth at late times. These two components only account for $\sim70$%\ of the scatter in mass accretions histories however, due to the stochastic effect of major mergers. Relating structural parameters to formation history, we find that concentration correlates strongly with the early history of the halo, while relaxation correlates with the late history. We examine the inferences about formation history that can be drawn by splitting haloes into subsamples, based on observable properties such as concentration and shape at some final time. This approach suggests interesting possibilities, such as the possibility of defining young and old samples of galaxy clusters in a rigorous, quantitative way, or testing the dynamical assumptions of galaxy formation models empirically.