BV CCD frames have been used to derive surface brightness profiles for
NGC 3201 which extend out to similar to 18'. A total of 857 radial ve
locities with median precision similar or equal to 1 km s(-1) for 399
member giants have been used to trace the velocity dispersion profile
out to 32.'1 (the approximate tidal radius determined from fits of sin
gle-mass, isotropic King-Michie models to the cluster surface brightne
ss profiles). The median difference in radial velocity for stars on ei
ther side of an imaginary axis stepped through the cluster in 1 degree
s increments shows a statistically significant maximum amplitude of 1.
22 +/- 0.25 km s(-1). We discuss several possible explanations of this
result, including (1) cluster rotation, (2) preferential stripping of
stars on prograde orbits near the limiting radius, (3) the projection
of the cluster space velocity onto the plane of the sky, and (4) a sl
ight drift in the velocity zero point. It is difficult to unambiguousl
y identify the primary cause of the observed structure in the velocity
field, however, and we suspect that all of the above processes may pl
ay a role. The BV surface brightness profiles and radial velocities ha
ve been modeled with both single- and multimass King-Michie models and
nonparametric techniques. The corresponding density profiles and M/L
profiles show good agreement over the interval 1.5 less than or simila
r to R less than or similar to 10 pc, and both approaches suggest a st
eady rise in M/L with distance from the cluster center. Due to the low
cluster luminosity we are unable to place useful constraints on the a
nisotropy of the velocity dispersion profile, although the global mass
-to-light ratio is well constrained by the models: M/L(B) similar or e
qual to M/L(V) similar or equal to 2.0 +/- 0.2 for the multimass and n
onparametric models, compared to similar or equal to 1.65 +/- 0.15 for
models having equal-mass stars. Our best-fit, multimass models have m
ass function slopes of x similar or equal to 0.75 +/- 0.25, consistent
with recent findings that the form of the mass function depends on th
e position relative to the potential of the Galaxy.