  Elements of kinematical and dynamical modeling of elliptical galaxies (Es)
are presented. In projection, NFW models resemble Sersic models, but with a
very narrow range of shapes (m=3+/-1). The total density profile of Es cannot
be NFW-like because the predicted local M/L and aperture velocity dispersion
within an effective radius (Re) are much lower than observed. Stars must then
dominate Es out to a few Re. Fitting an NFW model to the total density profile
of Sersic+NFW (stars+dark matter [DM]) Es results in very high concentration
parameters, as found by X-ray observers. Kinematical modeling of Es assuming an
isotropic NFW DM model underestimates M/L at the virial radius by a factor of
1.6 to 2.4, because dissipationless LCDM halos have slightly different density
profiles and slightly radial velocity anisotropy. In N-body+gas simulations of
Es as merger remnants of spirals embedded in DM halos, the slope of the DM
density profile is steeper when 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 (h_4) to infer anisotropy in Es is dangerous, as h_4 is also sensitive
to small levels of rotation. The stationary Jeans equation provides accurate
masses out to 8 Re. The discrepancy between the modeling of Romanowsky et al.
(2003), indicating a dearth of DM in Es, and the simulations analyzed by Dekel
et al. (2005), which match the spectroscopic observations of Es, is partly due
to radial anisotropy and to observing oblate Es face-on. However, one of the 15
solutions to the orbit modeling of Romanowsky et al. is found to have an amount
and concentration of DM consistent with LCDM predictions.
