  We discuss the intimate relationship between the filamentary features and the
rare dense compact cluster nodes in this network, via the large scale tidal
field going along with them, following the cosmic web theory developed Bond et
al. The Megaparsec scale tidal shear pattern is responsible for the contraction
of matter into filaments, and its link with the cluster locations can be
understood through the implied quadrupolar mass distribution in which the
clusters are to be found at the sites of the overdense patches. We present a
new technique for tracing the cosmic web, identifying planar walls, elongated
filaments and cluster nodes in the galaxy distribution. This will allow the
practical exploitation of the concept of the cosmic web towards identifying and
tracing the locations of the gaseous WHIM. These methods, the Delaunay
Tessellation Field Estimator (DTFE) and the Morphology Multiscale Filter (MMF)
find their basis in computational geometry and visualization.
