On the connectivity of the cosmic web: theory and implications for cosmology and galaxy formation. Issue 1 (21st June 2018)

• Record Type: Journal Article
• Authors: Codis, Sandrine; Pogosyan, Dmitri; Pichon, Christophe
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 479:Issue 1(2018)
• Page Start: 973
• Page End: 993
• Publication Date: 2018-06-21
• Subjects: methods: analytical -- methods: numerical -- galaxies: formation -- dark energy -- large-scale structure of Universe; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/sty1643
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Cosmic connectivity and multiplicity, i.e. the number of filaments globally or locally connected to a given cluster is a natural probe of the growth of structure and in particular of the nature of dark energy. It is also a critical ingredient driving the assembly history of galaxies as it controls mass and angular momentum accretion. The connectivity of the cosmic web is investigated here via the persistent skeleton. This tool identifies topologically the ridges of the cosmic landscape which allows us to investigate how the nodes of the cosmic web are connected together. When applied to Gaussian random fields corresponding to the high-redshift universe, it is found that on average the nodes are connected to exactly κ = 4 neighbours in two dimensions and ∼6.1 in three dimensions. Investigating spatial dimensions up to d = 6, typical departures from a cubic lattice κ = 2 d are shown to scale like the power 7/4 of the dimension. These numbers strongly depend on the height of the peaks: the higher the peak the larger the connectivity. Predictions from first principles based on peak theory are shown to reproduce well the connectivity and multiplicity of Gaussian random fields and cosmological simulations. As an illustration, connectivity is quantified in galaxy lensing convergence maps and large dark haloes catalogues. As a function of redshift and scale the mean connectivity decreases in a cosmology-dependent way. As a function of halo mass, it scales like 10/3 times the log of the mass. Implications on galactic scales are discussed.