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 ^ { -1 } at \sim 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,L _ { z } ) implied by the velocity data .