fits were performed using the (approximate) deprojection of the core-S´ersic model given by @Terzic05. When scaled by these core radii, the anisotropy profiles of the @Quinlan97 simulations are all very similar. They define the lower boundary of the shaded region in Figure \[fig:intrinsic\](a).

@Milosavljevic01 investigated the entire merging process of two identical elliptical galaxies with initial central density slopes $\gamma = -2$ and also measured core radii from the remnant’s final projected surface mass profile. Their definition of ${r_b}$ (radius of maximum curvature) differs slightly from our ${r_b}$ derived with core-S´ersic models, but the difference is small ($\sim 10$%). The results of @Milosavljevic01 define the upper boundary of the shaded area in Figure \[fig:intrinsic\](a).

Both simulations predict a transition in the orbital structure around the core radius: inside ${r_b}$, tangential orbits dominate; outside the core, radial orbits take over. Similar anisotropy patterns have been derived in other simulations as well [@Zier01; @Meiron10; @Antonini12].

The observed orbital structure of the core galaxies follows this prediction closely, while non-core galaxies do not exhibit the characteristic change in the orbital structure from tangential to radial anisotropy. This provides the first convincing dynamical evidence for core scouring in massive elliptical galaxies.

Mass Deficits and 