elliptical galaxies. All of our galaxies have high-resolution, adaptive-optics assisted, integral field (IFU) stellar kinematical data obtained with SINFONI at the European Southern Observatory Very Large Telescope (ESO-VLT). We use state-of-the-art axisymmetric orbit superposition models [@Schwarzschild79] that include the effects of a central SMBH, stars and a DM halo. Six of the galaxies are core galaxies, while five do not have detectable cores at the resolution limit of [[*HST*]{}]{} [@Rusli13a; @Rusli13b]. We compare the orbit distributions in both types of galaxies against each other and against predictions from core-formation models.

The paper is organized as follows. In Section \[sec:sample\], we present an overview of the galaxy sample, observations, and dynamical models. Anisotropies are described and compared with previous modeling results in Section \[sec:previous\]. In Section \[sec:orbits\], we compare our results quantitatively with core-formation models. The paper is summarized in Section \[sec:summary\].

[lcccccc]{} NGC1407 & $2.0$ & $2.0$ & $0.19$ & $4.5$ & $0.96$ & $276.1$\
NGC1550 & $1.2$ & $0.7$ & $0.17$ & $3.7$ & $2.95$ & $270.1$\
NGC3091 & $0.6$ & $0.6$ & $0.17$ & $3.6$ & $4.36$ & $297.2$\
NGC4472 & $1.8$ & $1.5$ & $0.47$ & $2.5$ & $1.46$ & $300.2$\
NGC5328 & $0.9$ & $0.7$ & 