only inside $r \la 0.2 \, {r_b}$. A direct comparison to our work is hampered by the fact that @Gebhardt11 do not fit a stellar M/L ratio but use the dynamical stellar M/L from @Murphy11, which was determined from kinematical data with lower central resolution. In addition to this difference in the modeling approach, the velocity dispersion profile of M87 rises steeply inside the core region, while our core galaxies have nearly constant central velocity dispersion profiles (cf. @Gebhardt11 and @Rusli13a).

The situation for power-law galaxies is less clear due to the complete lack of comparison galaxies studied based on IFU data and models similar to ours: the existing models with DM for non-core galaxies by @Schulze11 and the ones for NGC4594 [@Jardel11] are based on long-slit data. Our ${\beta_\mathrm{rot}}$ seem slightly less negative than the ones in Figure \[fig:dm\](d). Whether this is due to the use of IFU versus long-slit data is unclear. The published anisotropies of @Schulze11 are along the galaxies’ major axes, where the influence of $v_\varphi$ on the anisotropy is largest. This could also explain their more extreme tangential anisotropies, apart from intrinsic variations in the orbital structure among non-core galaxies, in which stellar orbits seem 