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We use an approach to estimate galaxy morphologies based on an ellipticity(e) vs. Bulge-to-Total ratio (B/T) plane. We have calibrated this plane bycomparing with Dressler's classifications. With the aid of our calibration, wehave classified 635 galaxies in 18 Abell clusters (0.02 < z < 0.08). Ourapproach allowed us to recover the Kormendy's relation. We found thatellipticals and Spirals are slightly brighter than S0 in R band. As S0 bulgesare brighter than spirals bulges, we believe that ram pressure is not the mainmechanism to generate S0s. In our sample, cluster radio galaxies morphologiescover the range S0-E-cD and their bulges have absolutes magnitudes distributedwithin -21 mag < M < -24.5 mag. If we believe Ferrarese & Merrit's relation,these radio sources have 10^8-10^9 M black hole mass.

Cluster Galaxy Morphologies: The Relationship among Structural Parameters, Activity and the Environment