Characterization of Omega-WINGS galaxy clusters. I. Stellar light and
  mass profiles
  Galaxy clusters are the largest virialized structures in the observable
Universe. The knowledge of their properties provides many useful astrophysical
and cosmological information.
  Our aim is to derive the luminosity and stellar mass profiles of the nearby
galaxy clusters of the Omega-WINGS survey and to study the main scaling
relations valid for such systems.
  We have merged the data of the WINGS and Omega-WINGS databases, sorted the
sources according to the distance from the brightest cluster galaxy (BCG) and
calculated the integrated luminosity profiles in the $B$ and $V$ bands, taking
into account extinction, photometric and spatial completeness, K-correction and
background contribution. Then, by exploiting the spectroscopic sample we
derived the stellar mass profiles of the clusters.
  We got the luminosity profiles of 46 galaxy clusters, reaching $r_{200}$ in
30 cases, and the stellar mass profiles of 42 of our objects. We successfully
fitted all the integrated luminosity growth profiles with one or two embedded
S\'ersic components, deriving the main clusters parameters.
  Finally, we checked the main scaling relation among the clusters parameters
in comparison with those obtained for a selected sample of early-type galaxies
(ETGs) of the same clusters.
  We found that the nearby galaxy clusters are non-homologous structures like
ETGs and exhibit a color-magnitude (CM) red-sequence relation very similar to
that observed for galaxies in clusters. These properties are not expected in
the current cluster formation scenarios. In particular the existence of a CM
relation for clusters, shown here for the first time, suggests that the
baryonic structures grow and evolve in a similar way at all scales.
