Clusters in the Disperse cosmic web
  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
$\leq$ 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.
