Characterising the Structure of Halo Merger Trees Using a Single Parameter: The Tree Entropy

TL;DR

This paper introduces the 'tree entropy' parameter to quantify dark matter halo assembly history, revealing its strong correlation with galaxy morphology and offering a new way to connect galaxy properties with halo merger structures.

Contribution

The paper defines a novel dimensionless parameter 'tree entropy' to characterize halo merger trees, linking halo assembly geometry to galaxy properties using simulations.

Findings

Distribution of s peaks near 0.4

s correlates with galaxy morphology more than other halo properties

Weak dependence of s on halo mass and redshift

Abstract

Linking the properties of galaxies to the assembly history of their dark matter haloes is a central aim of galaxy evolution theory. This paper introduces a dimensionless parameter $s\in[0,1]$, the "tree entropy", to parametrise the geometry of a halo's entire mass assembly hierarchy, building on a generalisation of Shannon's information entropy. By construction, the minimum entropy ($s=0$) corresponds to smoothly assembled haloes without any mergers. In contrast, the highest entropy ($s=1$) represents haloes grown purely by equal-mass binary mergers. Using simulated merger trees extracted from the cosmological $N$-body simulation SURFS, we compute the natural distribution of $s$, a skewed bell curve peaking near $s=0.4$. This distribution exhibits weak dependences on halo mass $M$ and redshift $z$, which can be reduced to a single dependence on the relative peak height $\delta_{\rm c}/\sigma(M,z)$ in the matter perturbation field. By exploring the correlations between $s$ and global galaxy properties generated by the SHARK semi-analytic model, we find that $s$ contains a significant amount of information on the morphology of galaxies $-$ in fact more information than the spin, concentration and assembly time of the halo. Therefore, the tree entropy provides an information-rich link between galaxies and their dark matter haloes.