  We use the distribution of gravitationally-lensed image separations observed
in the Cosmic Lens All-Sky Survey (CLASS) and the PMN-NVSS Extragalactic Lens
Survey (PANELS), which are (nearly) complete for the image separation range
$0''.3 \le \Delta \theta \le 6''$, to constrain a model velocity dispersion
function (VF) of early-type galaxies. Assuming a current concordance
cosmological model and adopting a singular isothermal ellipsoid (SIE) model for
galactic potentials, we consider constraining both a characteristic velocity
dispersion (parameter $\sigma_*$) and the shape of the function (parameters
$\alpha$ and $\beta$; Sheth et al. 2003) for $0.3 \la z \la 1 $. If all three
parameters are allowed to vary, then none of the parameters can be tightly
constrained by the lensing data because of the small size of the sample. If we
fix the shape of the function by either the SDSS local stellar VF or an
inferred local stellar VF based on the SSRS2 galaxy sample, then the
constrained values of $\sigma_*$ are nearly equal to the corresponding stellar
values; we have $f_{\rm SIE/center} (\equiv \sigma_{*{\rm SIE}}/\sigma_{*{\rm
center}})= 0.90\pm 0.18 {\rm (SDSS)}$ or $1.04 \pm 0.19 {\rm (SSRS2)}$ assuming
non-evolution of the function between the present epoch and $z \sim 0.6$.
Finally, using only the CLASS statistical sample (Browne et al. 2003) and thus
including an absolute multiple-imaging probability, we find that the SDSS
stellar VF may have significantly underestimated the abundance of
morphologically early-type galaxies.
