Large Scale Structure. The seventies & Forty years later: From Clusters
  to Clusters
  I describe the beginning, ~ 1970, of the spectroscopic redshift surveys and
the discovery of the superclusters filamentary structures and voids. This
changed the view of the distribution of luminous light from the way we knew it
at the end of the sixties, a uniform distribution of galaxies with clusters
superimposed, and the way we understood it during the seventies, clusters
imbedded in filamentary structures. We planned in brief to understand the
distribution of galaxies and the effect of their environment since to learn
about the formation and evolution of the Universe, we need to know first how it
is now. The very large surveys, first among these the CfA, started in the
eighties thanks also to dedicated telescopes; during that period, the
distribution of mass on large scales was also measured. A next step, in
addition to the many and deep galaxies survey that are going on, could be a
deep cluster survey to detect distant clusters, improve the accuracy of the
clusters physical parameters as a function of redshift and have a more robust
probe for Cosmology.
