(see above). Our models presented here are instead based on [*IFU*]{} spectroscopic data that fully cover the galaxy centers and provide the most complete constraint on stellar orbits.

![image](f3.eps)

The bottom row of Figure \[fig:nodm\] compiles previous anisotropy measurements, where those based on IFU data are again highlighted and referenced on the left, while models fitted to long-slit data are quoted on the right. Note that @Gebhardt07, @Gueltekin09, and @Schulze11 used ${\beta_\mathrm{rot}}$, while all other results shown in Figures \[fig:nodm\](c) and (d) are for $\beta$.

Core galaxy models without DM generally yield isotropic or even slightly radial orbit distributions (${\beta_\mathrm{rot}},\, \beta \ga 0$; Figure \[fig:nodm\](c)). According to Equation (\[eq:sigrot\]), ${\beta_\mathrm{rot}}$ is always lower than $\beta$. Thus, different definitions of $\beta$ cannot explain why many previous studies found isotropic or slightly radial orbit distributions in core galaxies (around ${r_b}$). But the inclusion of rotation can partly explain the difference among the non-core galaxies in Figure \[fig:nodm\](d). In any case, even with models that neglect DM halos, stellar orbits in power-law galaxies appear more strongly biased in the tangential direction than do those in core galaxies.

From Figure \[fig:dm\], it becomes clear that models that do include DM and a SMBH recover 