Multi-epoch observations with ACS and WFC3 on HST provide a unique and comprehensive probe of stellar dynamics within 47 Tucanae .
We confront analytic models of the globular cluster with the observed stellar proper motions that probe along the main sequence from just above 0.8 to 0.1M _ { \odot } as well as white dwarfs younger than one gigayear .
One field lies just beyond the half-light radius where dynamical models ( e.g . lowered Maxwellian distributions ) make robust predictions for the stellar proper motions .
The observed proper motions in this outer field show evidence for anisotropy in the velocity distribution as well as skewness ; the latter is evidence of rotation .
The measured velocity dispersions and surface brightness distributions agree in detail with a rotating , anisotropic model of the stellar distribution function with mild dependence of the proper-motion dispersion on mass .
However , the best fitting models under-predict the rotation and skewness of the stellar velocities .
In the second field , centered on the core of the cluster , the mass segregation in proper motion is much stronger .
Nevertheless the model developed in the outer field can be extended inward by taking this mass segregation into account in a heuristic fashion .
The proper motions of the main-sequence stars yield a mass estimate of the cluster of 1.31 \pm 0.02 \times 10 ^ { 6 } \mathrm { M } _ { \odot } at a distance of 4.7 kpc .
By comparing the proper motions of a sample of giant and sub-giant stars with the observed radial velocities we estimate the distance to the cluster kinematically to be 4.29 \pm 0.47 kpc .