  We analyse a sample of about 2000 galaxies in 40 regular clusters, to look
for evidence of segregation with respect to galaxy luminosities and
morphological types. We find evidence of luminosity segregation for galaxies
brighter than $M_R < -21.5$, i.e. typically the four brightest members of each
cluster. We also find evidence of morphological segregation: both the
core-radius and the velocity dispersion increase along the Hubble sequence
(ellipticals - S0 - early spirals - late spirals). Galaxies of different types
have different velocity dispersion profiles, being steeper for later type
galaxies. Simple modelling allows us to show that elliptical (and, to a lesser
extent, S0) orbits are mostly tangential in the cluster core, and nearly
isotropic outside, while spiral (in particular late-spiral) orbits are
predominantly radial. A viable interpretation of our results is that (1) late
spirals, at variance with other type galaxies, are a non-virialized cluster
population, still on partially radial infalling orbits, (2) the elliptical
phase-space distribution is evolving towards energy equipartition through the
process of dynamical friction, (3) S0 and early-spirals have intermediate
distributions between these two extremes.
