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Models satisfying the above assumptions fit the observations of all four galaxies remarkably well.
For all galaxies the rotation curves rule out isotropic velocity dispersion tensors. However, an excellent fit to the data can usually be obtained by including a measure of velocity anisotropy. Only in the case of NGC 4472 do the velocity dispersion profiles suggest that the radial and vertical dispersions are decoupled and thus the distribution function depends upon a third integral. Such behaviour is allowed by our models but since it is associated with a large isophote twist, it likely indicates a triaxial figure. In boxy galaxies the rotation velocity falls more slowly away from the equatorial plane than in the equivalent disky galaxies.