and (d). Models based on IFU data are highlighted and referenced on the left, while models fitted to long-slit data are quoted on the right. All models shown in Figure \[fig:dm\] include a SMBH, stars, and a DM halo.

The core-galaxy models of @Schulze11 do not show a tendency toward tangential anisotropy inside the core radius ${r_b}$: instead, all three core galaxies in their sample (NGC3608, NGC4291, and NGC4649) show nearly constant and isotropic dispersion profiles (Figure \[fig:dm\](c)). The recent models of the two brightest cluster galaxies NGC3842 and NGC7768 [@McConnell12][^2] do show increasing tangential anisotropy, as do our models. We attribute the different results to the different data that were used: @Schulze11 use long-slit [[*HST*]{}]{} data that do not fully cover the central galaxy regions and leave most stellar orbits unconstrained. In contrast, the study of @McConnell12 and ours are based on IFU spectroscopic data in the center that provide full spatial coverage and the most complete constraints on stellar orbits. This indicates that IFU data are important for understanding the central orbital structure in core galaxies. However, we note that the latest model of M87 by @Gebhardt11 is based on IFU data as well. It shows tangential anisotropy 