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: http://www.stsci.edu/~marel/abstracts/abs_R15.html
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The dependence of the intrinsic and projected properties on the model parameters and the inclination is described. The case I models have a larger ratio of RMS tangential to radial motion in the equatorial plane than on the symmetry axis, the more so for smaller axial ratios. The case II models have a constant ratio of RMS tangential to radial motion throughout the system, as characterized by Binney's parameter beta. The maximum possible ratio v/sigma of the mean projected line-of-sight velocity and velocity dispersion on the projected major axis always decreases with increasing radial anisotropy. The observed ratio of the RMS projected line-of-sight velocities on the projected major and minor axes of elliptical galaxies is best fit by the case II models with beta > 0. These models also predict non-Gaussian velocity profile shapes consistent with existing observations.
The distribution functions are used to model the galaxies NGC 2434
(E1) and NGC 3706 (E4), for which stellar kinematical measurements out
to two effective radii indicate the presence of dark halos (Carollo et al.). The velocity profile shapes
of both galaxies can be well fit by radially anisotropic case II
models with a spherical logarithmic potential. This contrasts with the
f(E,L_z) models studied previously, which require flattened dark halos
to fit the data.