Galaxy Morphology in the Virgo Cluster and in the de Vaucouleurs Groups

We find a 13%-14% elliptical fraction in the classical de Vaucouleurs groups and in the Virgo cluster except in the cluster core where the elliptical and SO fractions are both significantly enhanced. There are no significant differences between the morphological fractions in the Virgo cluster as a whole and the groups. There is no significant Virgocentric radial variation in the de Vaucouleurs group morphological fractions. This supports the assertion that the Virgo cluster as a whole and the groups formed with the same morphological fractions. The data are consistent with the Whitmore, Gilmore, and Jones scenario in which tidal forces in cluster cores limit bright spiral galaxy formation there. It is also consistent with the spiral-merger scenario in which the initial morphological fractions are the same in the groups and the cluster, some spirals in the cluster core merge to form ellipticals, and other spirals are converted into S0's by gas stripping.