structure: at $\alpha=0$, the entropy is maximized, while for larger $\alpha$, the orbital weights are adjusted more to fit the model to the kinematical observations (as good as the actual trial potential allows). The results presented in this paper are based on models with maximum $\alpha$, i.e., the orbit distribution is entirely determined by the observational data. A detailed description of our implementation of the Schwarzschild method can be found in @Thomas04 [@Thomas05].

![image](f1.eps)

Stellar orbits in the centers\
of massive ellipticals {#sec:previous}
==============================

Figures \[fig:dm\](a) and (b) show the distribution of stellar orbits in our galaxies as measured from the best-fit models. The figure shows for each galaxy the radial profile of the orbital anisotropy parameter: $$\label{eq:betarot}
{\beta_\mathrm{rot}}= 1 - \frac{\sigma_\mathrm{rot}^2}{\sigma_r^2},$$ where $$\label{eq:sigrot}
\sigma_\mathrm{rot}^2 = (\sigma^2_\vartheta + \sigma^2_\varphi + v_\varphi^2
)/2$$ is the light-weighted spherically averaged second velocity moment in the tangential direction and $\sigma_r$ the corresponding moment in the radial direction. In Figure \[fig:dm\](a), the radial coordinate is scaled by the core radius ${r_b}$ and only core galaxies are shown. In Figure \[fig:dm\](b), only the non-core galaxies are shown and the radial coordinate is scaled by the sphere-of-influence radius ${r_\mathrm{soi}}= G\,{M_\bullet}/\sigma_e^2$. In our core galaxies ${r_\mathrm{soi}}\sim
{r_b}$ (Table 