  A simple algorithm is presented for the calculation of the projected
line-of-sight velocity profiles (VPs) of non-rotating anisotropic spherical
stellar dynamical models with a phase-space distribution function of the
Osipkov-Merritt type. The velocity distribution in these models is isotropic
inside the anisotropy radius r_a and becomes increasingly radially biased at
larger radii. VP shape parameters are presented for a family of models in which
the luminous mass density has an r^{-gamma} power-law cusp at small radii and
an r^{-4} power-law fall-off at large radii. Self-consistent models and models
in which the luminous matter is embedded in a dark halo are discussed. The
effects of changes in the cusp slope gamma and in the anisotropy radius r_a are
documented, and the area in the (gamma,r_a)-plane that contains physical models
is delineated. The shapes of the VPs of the models show a considerable (and
observable) variation with projected galactocentric radius. These models will
be useful for interpreting the data on the VP shapes of elliptical galaxies
that are now becoming available.
