Distribution of our lens models as a function of the dark matter slope and H₀. The colour code gives the value of (see text; Eq. (7)). Only the models with are shown. The results in the left panel are for a Salpeter IMF, and for a Kroupa IMF in the right panel. The lensing χ² itself is not included in the figure. However, it is systematically lower for galaxies with Kroupa IMFs than for galaxies with Salpeter IMFs.