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The Tessellation-Level-Tree: characterizing the nested hierarchy of density peaks and their spatial distribution in cosmological N-body simulations

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Busch,  Philipp
Computational Structure Formation, MPI for Astrophysics, Max Planck Society;

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White,  Simon D. M.
Computational Structure Formation, MPI for Astrophysics, Max Planck Society;

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Citation

Busch, P., & White, S. D. M. (2020). The Tessellation-Level-Tree: characterizing the nested hierarchy of density peaks and their spatial distribution in cosmological N-body simulations. Monthly Notices of the Royal Astronomical Society, 493(4), 5693-5712. doi:10.1093/mnras/staa572.


Cite as: http://hdl.handle.net/21.11116/0000-0006-BDA5-B
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 ∼80⟨ρ⟩ results in a structure similar to a standard friend-of-friends halo and its subhaloes. For thresholds below ∼7⟨ρ⟩⁠, 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⟨ρ⟩⁠, it contains about half of all cosmic mass and occupies ∼1 per cent of all cosmic volume; a typical external point is then ∼7h−1 Mpc from the web. We investigate the internal structure and clustering of tlt peaks. Defining the saddle point density ρlim  as the density at which a peak joins its parent peak, we show the median value of ρlim   for FoF-like peaks to be similar to the density threshold at percolation. Assembly bias as a function of ρlim   is stronger than for any known internal halo property. For peaks of group mass and below, the lowest quintile in ρlim    has b ≈ 0, and is thus uncorrelated with the mass distribution.