  Scaling relations among dark matter (DM) and stellar quantities are a
valuable tool to constrain formation scenarios and the evolution of galactic
structures. However, most of the DM properties are actually not directly
measured, but derived through model dependent mass mapping procedures. It is
therefore crucial to adopt theoretically and observationally well founded
models. We use here an updated version of the secondary infall model (SIM) to
predict the halo density profile, taking into account the effects of angular
momentum, dissipative friction and baryons collapse. The resulting family of
halo profiles depends on one parameter only, the virial mass, and nicely fits
the projected mass and aperture velocity dispersion of a sample of intermediate
redshift lens galaxies. We derive DM related quantities (namely the column
density and the Newtonian acceleration) and investigate their correlations with
stellar mass, luminosity, effective radius and virial mass.
