\[tab:data\]).

Homology in the Velocity Dispersion Tensor
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The dynamical structure around the SMBHs in core galaxies is different from that in non-core, power-law galaxies. The central anisotropy profiles of the six core galaxies are remarkably uniform. Stellar motions inside the core radius ${r_b}$ are strongly dominated by tangential orbits (${\beta_\mathrm{rot}}<0$), while outside ${r_b}$ radial orbits quickly take over (${\beta_\mathrm{rot}}>0$). In fact, there is a strong homology in the anisotropy profiles: when scaled by the core radius $r_b$, the radial profiles of the classical anisotropy parameter ${\beta_\mathrm{rot}}(r)$ are nearly identical in core galaxies. The five galaxies without cores do not show any coherent anisotropy pattern, but instead are tangentially biased on all spatial scales.

The homogeneity of the stellar orbits is not directly enforced by the break in the light profiles. To check this, we also built maximum-entropy models [e.g. @Thomas09] for each core galaxy. These models reproduce the light profile equally well but are isotropic in the center. They do not fit the observed kinematics, however, having higher central velocity dispersions and steeper velocity dispersion gradients than observed.

Previous Anisotropy Measurements
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A compilation of previous anisotropy measurements in the centers of early-type galaxies is shown in Figures \[fig:dm\](c) 