  The stellar dynamics of Omega Centauri are inferred from the radial
velocities of 469 stars measured with CORAVEL (Mayor et al. 1997). Rather than
fit the data to a family of models, we generate estimates of all dynamical
functions nonparametrically, by direct operation on the data. The cluster is
assumed to be oblate and edge-on but mass is not assumed to follow light. The
mean motions are consistent with axisymmetry but the rotation is not
cylindrical. The peak rotational velocity is 7.9 km/s at 11 pc from the center.
The apparent rotation of Omega Centauri is attributable in part to its proper
motion. We reconstruct the stellar velocity ellipsoid as a function of
position, assuming isotropy in the meridional plane. We find no significant
evidence for a difference between the velocity dispersions parallel and
perpendicular to the meridional plane. The mass distribution inferred from the
kinematics is slightly more extended than, though not strongly inconsistent
with, the luminosity distribution. We also derive the two-integral distribution
function f(E,Lz) implied by the velocity data.
