All Tables

Table 1: Results for the SIS model for different lens samples and $r_{\rm max}=150h^{-1}~{\rm kpc}$ . $N_{\rm d}$ , $N_{\rm s}$ and $N_{\rm p}$ are the numbers of lenses, sources and pairs in each measurement. Note that the number of sources can vary for different lens selections because not all source candidates are always lying within $r_{\rm max}$ of a lens. The best fit values of $\sigma _*$ and $\eta$ are given with 1- $\sigma$ error bars. The last two columns give the aperture mass within $150h^{-1}~{\rm kpc}$ and the corresponding mass-to-light ratio.
Table 2: Constraints on dark matter halos of galaxies modelled by NFW profiles for different lens samples and $r_{\rm max}=400h^{-1}~{\rm kpc}$ . $N_{\rm d}$ , $N_{\rm s}$ and $N_{\rm p}$ are the numbers of lenses, sources and pairs in each measurement. These numbers differ from those given in Table 1 because of the larger $r_{\rm max}$ used here. The virial radius $r_{\rm vir}^*$ and $\alpha$ are fitted quantities (see Fig. 4), the virial mass $M_{\rm vir}^*$ and the virial mass-to-light ratio $M_{\rm vir}^*/L^*$ are calculated from $r_{\rm vir}^*$ . $\beta =3\alpha -1$ gives the scaling of $M_{\rm vir}/L$ with luminosity, $M_{\rm vir}/L\propto L^\beta$ . All errors are 1- $\sigma$ .
Table 3: Central positions, redshifts and velocity dispersions of the known clusters in the A 901 field (Taylor et al. 2004).