exist in axisymmetric potentials. However, the associated radial anisotropies in the triaxial models of NGC3379 and NGC3998 are similar to those in other galaxies derived from similar data and assumptions about the mass profile (no DM halo). Moreover, the triaxial model of NGC3379 is similar to the axisymmetric model of NGC3379 by @Shapiro06 outside $r \ga {r_b}/2$. NGC3379 and NGC3998 thus do not provide evidence that the assumption of axial symmetry induces a strong bias. This could be expected for the central regions where the potential is dominated by the SMBH, i.e., spherical and Keplerian. Final conclusions can only be drawn when triaxial models with a DM halo are available.

The orbit distributions derived for the centers of power-law galaxies are probably more uncertain than those for core galaxies. At the innermost resolved data point there are still orbits with pericenters at even smaller radii. These orbits are only partly constrained, by light scattered from the center to larger radii through point-spread function effects. Because power-law galaxies have brighter centers, constraints from presently unresolved spatial regions are likely to affect dynamical models more strongly than in core galaxies with their faint inner regions.

Core formation {#sec:orbits}
==============

The remarkable homogeneity 