All Figures

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{4142_fig1.eps}} \end{figure}$ Figure 1: Image magnifications. Solid line: the brighter images ( $\mu _+(y)$ , x>0), dashed line: the fainter images ( $\mu _-(y)$ , x<0). The left vertical line (dot-dashed) indicates the source position $y_{{\rm cr}}$ at which $q_{\rm r}=10$ , and the right vertical line (dotted) indicates the position for $q_{\rm r}=10^{4}$ .
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics{4142_fig2.eps}} \end{figure}$ Figure 2: The integral lensing probabilities with image separations larger than $\Delta \theta$ and flux density ratio less than $q_{{\rm r}}$ , for quasars at mean redshift $\langle z_{\rm s}\rangle =1.27$ lensed by NFW ( $M_{\rm DM}>M_{\rm c}$ ) and SIS+SMBH ( $M_{\rm DM}<M_{\rm c}$ ) halos. The typically selected values of the cosmic equation of state $\omega$ for each curve, the flux density ratio $q_{{\rm r}}$ and cooling scale $M_{\rm c}$ are explicitly indicated. The observed lensing probabilities of JVAS/CLASS are plotted as a histogram in each panel.
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{4142_fig1.eps}} \end{figure}$	Figure 1: Image magnifications. Solid line: the brighter images ( $\mu _+(y)$ , x>0), dashed line: the fainter images ( $\mu _-(y)$ , x<0). The left vertical line (dot-dashed) indicates the source position $y_{{\rm cr}}$ at which $q_{\rm r}=10$ , and the right vertical line (dotted) indicates the position for $q_{\rm r}=10^{4}$ .
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