The Tessellation-Level-Tree: characterizing the nested hierarchy of density peaks and their spatial distribution in cosmological N-body simulations. Issue 4 (28th February 2020)

• Record Type: Journal Article
• Authors: Busch, Philipp; White, Simon D M
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 493:Issue 4(2020)
• Page Start: 5693
• Page End: 5712
• Publication Date: 2020-02-28
• Subjects: methods: data analysis -- large-scale structure of Universe; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa572
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We use the Millennium and Millennium-II simulations to illustrate the Tessellation-Level-Tree (tlt ), a hierarchical tree structure linking density peaks in a field constructed by voronoi tessellation of the particles in a cosmological N-body simulation. The tlt uniquely partitions the simulation particles into disjoint subsets, each associated with a local density peak. Each peak is a subpeak of a unique higher peak. The tlt can be persistence filtered to suppress peaks produced by discreteness noise. Thresholding a peak's particle list at $\sim 80\left \langle \rho \right \rangle \, $ results in a structure similar to a standard friend-of-friends halo and its subhaloes. For thresholds below $\sim 7\left \langle \rho \right \rangle \, $, the largest structure percolates and is much more massive than other objects. It may be considered as defining the cosmic web. For a threshold of $5\left \langle \rho \right \rangle \, $, it contains about half of all cosmic mass and occupies $\sim 1{{\ \rm per\ cent}}$ of all cosmic volume; a typical external point is then ∼7 h −1 Mpc from the web. We investigate the internal structure and clustering of tlt peaks. Defining the saddle point density ρl im as the density at which a peak joins its parent peak, we show the median value of ρl im for FoF-like peaks to be similar to the density threshold at percolation. Assembly bias as a function of ρl im is stronger than for any known internal halo property. For peaks of group mass and below, the lowest quintile in ρl im has b ≈ 0, and is thus uncorrelated with the mass distribution.