  We describe the Bayesian BARCODE formalism that has been designed towards the
reconstruction of the Cosmic Web in a given volume on the basis of the sampled
galaxy cluster distribution. Based on the realization that the massive compact
clusters are responsible for the major share of the large scale tidal force
field shaping the anisotropic and in particular filamentary features in the
Cosmic Web. Given the nonlinearity of the constraints imposed by the cluster
configurations, we resort to a state-of-the-art constrained reconstruction
technique to find a proper statistically sampled realization of the original
initial density and velocity field in the same cosmic region. Ultimately, the
subsequent gravitational evolution of these initial conditions towards the
implied Cosmic Web configuration can be followed on the basis of a proper
analytical model or an N-body computer simulation. The BARCODE formalism
includes an implicit treatment for redshift space distortions. This enables a
direct reconstruction on the basis of observational data, without the need for
a correction of redshift space artifacts. In this contribution we provide a
general overview of the the Cosmic Web connection with clusters and a
description of the Bayesian BARCODE formalism. We conclude with a presentation
of its successful workings with respect to test runs based on a simulated large
scale matter distribution, in physical space as well as in redshift space.
