  We present VLA observations of the distribution and kinematics of the HI gas
in the classical ring galaxy VIIZw466 and its immediate surroundings. The HI
gas corresponding to the bright optical star forming ring exhibits the typical
profile of a rotating-expanding ring. The systemic velocity of the galaxy is
found to be 14,468km/s. A formal fit to the HI kinematics in the ring is
consistent with both ring rotation and expansion (expansion velocity 32 km/s).
However, H\,I in the northeast quadrant of the ring is severely disturbed,
showing evidence of tidal interaction. We also detect a hydrogen plume from the
southern edge-on companion galaxy (G2) pointing towards the ring galaxy. This,
and other peculiarities associated with G2 suggest that it is the intruder
galaxy which recently collided with VIIZw466 and formed the ring. Numerical
hydrodynamic models are presented which show that most of the observed features
can be accounted for as a result of the impact splash between two gas disks.
The resultant debris is stretched by ring wave motion in the bridge and later
forms accretion streams onto the two galaxies.Finally, we detect HI emission
from two previously unknown dwarf galaxies located northeast and southeast of
VIIZw466 respectively. This brings the total number of members of the VIIZw466
group to five. Using the projected mass method, the upper limit of the
dynamical mass of the group was estimated to be Mo =3.5x10^{12} M_sun, which
implies that the mass to light ratio of the group is (M/L)_{group} \approx$ 70.
This rather low value of M/L, as compared with other loose groups, suggests the
group may be in a state of collapse at the present time. Plunging orbits would
naturally lead to an enhanced probability of head-on collisions and ring galaxy
formation.
