Elements of kinematical and dynamical modeling of elliptical galaxies arepresented.In projection, NFW models resemble Sérsic models, but with a very narrow range of shapes (m = 3±1).The total density profile of ellipticals cannot be NFW-like because the predicted local M/L and aperture velocity dispersion within aneffective radius (Re) are much lower than observed. Stars must then dominate ellipticalsout to a few Re.Fitting an NFW model to the total density profile of Sérsic+NFW (stars+dark matter [DM]) ellipticals results in very high concentration parameters, asfoundby X-ray observers.Kinematical modeling of ellipticals assuming an isotropic NFW DM modelunderestimates M/L at the virial radius by a factor of 1.6 to 2.4, becausedissipationless ΛCDM halos have slightly different density profilesand slightly radial velocity anisotropy. In N-body+gas simulations of ellipticals as merger remnants ofspirals embedded in DM halos,the slope of the DM density profile is steeperwhen the initial spiral galaxies are gas-rich.The Hansen & Moore (2006)relation between anisotropy and the slope of the density profile breaks down for gas and DM, but the stars follow an analogous relation with slightly less radial anisotropies for a given density slope.Using kurtosis (h4) to infer anisotropy in ellipticals is dangerous, as h4 is also sensitive to small levels of rotation.The stationary Jeans equation provides accurate masses out to 8Re.The discrepancy between the modeling of Romanowsky et al. (2003),indicating a dearth of DM in ellipticals,and the simulations analyzed by Dekel et al. (2005), whichmatch thespectroscopic observations of ellipticals, is partly due to radial anisotropy and to observing oblate ellipticals face-on.However,one of the 15 solutions to the orbit modeling of Romanowsky et al. is found to have an amount andconcentration ofDMconsistent withΛCDM predictions.