$0.14$ & $4.7$ & $5.70$ & $332.9$\
NGC7619 & $0.5$ & $0.4$ & $0.18$ & $2.5$ & $5.40$ & $292.2$\
NGC1374 & $\ldots$ & $0.8$ & $0.15$ & $0.6$ & $\ldots$ & $166.8$\
NGC4751 & $\ldots$ & $0.4$ & $0.22$ & $1.4$ & $\ldots$ & $355.4$\
NGC6861 & $\ldots$ & $0.4$ & $0.38$ & $2.0$ & $\ldots$ & $388.8$\
NGC307 & $\ldots$ & $0.2$ & $0.17$ & $0.6$ & $\ldots$ & $201.4$\
NGC1332 & $\ldots$ & $0.4$ & $0.14$ & $1.4$ & $\ldots$ & $292.4$\

Observations and Modeling {#sec:sample}
=========================

Our galaxy sample is based on the set of high velocity-dispersion ellipticals in @Rusli13a where we study the influence of DM halos on dynamical black hole mass measurements. Details of the photometric and kinematical data, the data reduction, and our modeling technique are presented therein. We observed the center of each galaxy with SINFONI at the ESO-VLT. These very high spatial resolution data guarantee that the sphere of influence of the central black hole is well resolved (Table \[tab:data\]). We combined these data with kinematical observations on larger scales, typically out to about the half-light radius of each galaxy. Extended spatial coverage with kinematical data is essential to constrain the 