  Determining which between projected local density and distance from the
cluster center plays a major role in regulating morphological fractions in
clusters is a longstanding debate. Reaching a definitive answer will shed light
on the main physical mechanisms at play in the most extreme environments. Here
we make use of the data from the OmegaWINGS survey, currently the largest
survey of clusters in the local Universe extending beyond 2 virial radii from
the cluster cores, to extend previous analysis outside the virial radius. Local
density and clustercentric distance seems to play different roles for galaxies
of different morphology: the fraction of elliptical galaxies mainly depends on
local density, suggesting that their formation was linked to the primordial
densities, which now correspond to the cluster cores. Only the fraction of low
mass ellipticals shows an anticorrelation with clustercentric distance,
suggesting a different origin for these objects. Excluding elliptical galaxies,
the relative fraction of S0s and spirals instead depends on local density only
far from the cluster cores, while within the virial radius their proportion is
regulated by distance, suggesting that cluster specific processes halt the star
formation and transform Sp galaxies into S0s. This interpretation is supported
by literature results on the kinematical analysis of early and late type
galaxies, according to which fast and slow rotators have distinct dependencies
on halo mass and local density.
