Clusters in the Disperse cosmic web

Abstract

Galaxy cluster mass halos ("clusters") in a dark matter simulation are matched to nodes in several different cosmic webs found using the Disperse cosmic web finder. The webs have different simulation smoothings and Disperse parameter choices; for each, 4 methods are considered for matching Disperse nodes to clusters. For most of the webs, Disperse nodes outnumber clusters, but not every cluster has a Disperse node match (and sometimes $>1$ cluster matches to the same Disperse node). The clusters frequently lacking a matching Disperse node have a different distribution of local shear trends and perhaps merger histories. It might be interesting to see in what other ways, e.g., observational properties, these clusters differ. For the webs with smoothing $\le$ 2.5 $Mpc/h$, and all but the most restrictive matching criterion, $\sim$3/4 of the clusters always have a Disperse node counterpart. The nearest cluster to a given Disperse node and vice versa, within twice the smoothing length, obey a cluster mass-Disperse node density relation. Cluster pairs where both clusters match Disperse nodes can also be assigned the filaments between those nodes, but as the web and matching methods are varied, most such filaments do not remain. There is an enhancement of subhalo counts and halo mass between cluster pairs, averaging over cluster pairs assigned Disperse filaments increases the enhancement. The approach here also lends itself to comparing nodes across many cosmic web constructions, using the fixed underlying cluster distribution to make a correspondence.

15 pages, 15 Figures. Revised version incorporating many helpful suggestions from the referee; more information about nodes matched or not to clusters, cluster pair profile quantities changed

References in corpus (8)

• Properties of Dark Matter Haloes in Clusters, Filaments, Sheets and Voids
• The Evolution of Dark Matter Halo Properties in Clusters, Filaments, Sheets and Voids
• Cosmological constraints from the CFHTLenS shear measurements using a new, accurate and flexible way of predicting nonlinear mass clustering
• Caught in the cosmic web: Environmental effect on halo concentrations, shape, and spin
• The Imprint of Cosmic Web Quenching on Central Galaxies
• The Persistent Percolation of Single-Stream Voids
• A comparison of cosmological filaments catalogues
• A robust determination of halo environment in the cosmic field

Cited by in corpus (3)

• The probability of identifying the cosmic web environment of galaxies around clusters motivated by the Weave Wide Field Cluster Survey
• The Three Hundred project: Estimating the dependence of gas filaments on the mass of galaxy clusters
• A first look at the topology of reionization redshifts in models of the Epoch of the Reionization