Clusters in the <scp>Disperse</scp> cosmic web

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