  For 89 galaxies, mostly spirals, in the Virgo cluster region, we have
obtained optical long-slit major axis spectra of the ionized gas. We find: (1)
One-half of the Virgo galaxies we observed have regular rotation patterns,
while the other 50% exhibit kinematic disturbances ranging from mild to major.
Velocity complexities are generally consistent with those resulting from tidal
encounters or accretion events. Since kinematic disturbances are expected to
fade within ~10^9 years, many Virgo galaxies have experienced several
significant kinematic disturbances during their lifetimes. (2) A few Virgo
galaxies have ionized gas of limited extent, with velocities exceptionally low
for their luminosities. In these galaxies the gas must be not rotationally
supported. (3) There is a remarkable difference in the distribution of galaxy
systemic velocity for galaxies with Regular rotation curves and galaxies with
Disturbed rotation curves. Galaxies with regular rotation patterns show a flat
distribution with systemic velocity, while galaxies with disturbed kinematics
have a Gaussian distribution very similar to that for the elliptical galaxies
in Virgo. This suggests that spirals with disturbed kinematics are
preferentially on radial orbits, which bring them to the cluster core, where
tidal interactions are strong and/or more common. These interactions may alter
the morphology of the galaxy, and may also play a role in driving the Virgo
cluster toward dynamical equilibrium.
