Gravitational lensing by CDM halos: singular versus nonsingular profiles

The gravitational lensing properties of cosmological halos depend upon the mass distribution within each halo. The description of halos as nonsingular, truncated isothermal spheres, a particular solution of the isothermal Lane-Emden equation (suitably modified for Λ 6= 0), has proved to be a useful approximation for the halos which form from realistic initial conditions in a CDM universe. The nonsingular TIS model reproduces many of the quantitative features of the N-body results for CDM halos, except in the very center, where CDM N-body halos show density profiles which vary as ρ ∼ r−α, α & 1, instead of a small flat core. Possible discrepancies between these cuspy halo predictions of the CDM N-body simulations and observations of the inner mass profiles of dwarf and LSB disk galaxies based upon their rotation curves and of clusters based upon strong lensing measurements have led to a search for other diagnostics. A description of the lensing by TIS halos would be useful in this regard, as a selfconsistent model for CDM halos in a proper cosmological context, nonsingular but otherwise consistent with the CDM N-body results. We derive here the basic lensing properties of individual TIS halos. For comparison, we also consider three singular profiles: the Navarro-Frenk-White density profile, the singular isothermal sphere, and the Schwarzschild lens. For all profiles, we compute the critical curves and caustics, the image separation, the magnification and brightness ratio, the shear, the time delay, and the average shear inside the tidal radius. This provides tools for studying the statistical properties of lensing by TIS and other lenses in the context of a theory of cosmological structure formation.