All Figures

$\begin{figure} \par\resizebox{8.7cm}{!}{\fbox{\includegraphics{1432f1.ps}}} \end{figure}$ Figure 1: A finding chart for FBQ 0951+2635. The star used to model the point spread function (PSF) is indicated. The two reference stars (labeled S2 and S3) used for the photometry are also marked.
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In the text

$\begin{figure} \par\mbox{\fbox{\includegraphics[width=4.1cm]{1432f2a.ps}} \fbox{\includegraphics[width=4.1cm]{1432f2b.ps}} } \end{figure}$ Figure 2: Left: stacked R-band image of a $12\hbox {$^{\prime \prime }$ }$ $\times$ $12\hbox {$^{\prime \prime }$ }$ region centered on FBQ 0951+2635. The seeing is $\sim$ 1 $\hbox{$.\!\!^{\prime\prime}$ }2$ and the total exposure time is $\sim$ 8.3 h. Right: deconvolved image ( FWHM = $0\hbox{$.\!\!^{\prime\prime}$ }28$ ) obtained from the simultaneous deconvolution of 49 frames. North is up and east to the left.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1432f3.ps} \end{figure}$ Figure 3: The A and B component R-band light curves for FBQ 0951+2635 and two reference stars in the field. The plotted values are R - 0.9 for B, R - 1.8 for S2 and R - 2.0 for S3. The magnitudes are calculated relative to the calibrated PSF star in the field. The error bars represent photon noise and PSF errors estimated from the deconvolution of the two reference stars. Since S2 and S3 are significantly fainter than components A and B, their photon noise is larger. The dashed horizontal lines represent the mean magnitudes of stars S2 and S3.
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In the text

$\begin{figure} \par\includegraphics[width=8.65cm,clip]{1432f4a.ps}\vspace*{4mm} ... ...4b.ps}\vspace*{4mm} \includegraphics[width=8.65cm,clip]{1432f4c.ps} \end{figure}$ Figure 4: Top: a zoom in on the light curves produced from the latest observations. The plotted values are R-0.9 for the B component in order to ease the comparison. A short-lived dip in the light curves is indicated by the two circles. Middle: time-delay shifted light curves of FBQ 0951+2635. B is shifted by +1.01 mag and forward in time by 17 days. A linear correction for the external variations is applied. Bottom: time-delay shifted light curves of FBQ 0951+2635. B is shifted by +1.06 mag and forward in time by 16 days. Only the last 38 data points were used with a direct method (no correction for external variations).
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8.65cm]{1432f5a.ps} \includegraphics[width=8.65cm]{1432f5b.ps} } \end{figure}$ Figure 5: Left: an HST/NICMOS image of FBQ 0951+2635. Right: a deconvolved HST/NICMOS image shown on a logarithmic intensity scale. In both panels the lensing galaxy is denoted by the letter "G''.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip,clip]{1432f6.ps} \end{figure}$ Figure 6: $\Delta \chi ^2$ contours for FBQ 0951+2635 in the plane of the ellipticity (e) and shear ( $\gamma$ ). The contours are drawn at $\Delta \chi ^2$ = 2.30, 6.17 and 11.8, corresponding to the $1 \sigma$ , $2 \sigma$ and $3 \sigma$ confidence intervals for two degrees of freedom. There is a weak degeneracy between e and $\gamma$ . The area between the horizontal dashed lines is the range of the measured ellipticity.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{1432f7.ps} \end{figure}$ Figure 7: Top: the slope of the projected mass density profile plotted against H₀ for 121 different non-parametric models. Bottom: probability distribution of the derived H₀ values for the same models as above. The median value of the distribution is indicated by the dotted line.
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In the text

$\begin{figure} \par\resizebox{8.7cm}{!}{\fbox{\includegraphics{1432f1.ps}}} \end{figure}$	Figure 1: A finding chart for FBQ 0951+2635. The star used to model the point spread function (PSF) is indicated. The two reference stars (labeled S2 and S3) used for the photometry are also marked.
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$\begin{figure} \par\mbox{\includegraphics[width=8.65cm]{1432f5a.ps} \includegraphics[width=8.65cm]{1432f5b.ps} } \end{figure}$	Figure 5: Left: an HST/NICMOS image of FBQ 0951+2635. Right: a deconvolved HST/NICMOS image shown on a logarithmic intensity scale. In both panels the lensing galaxy is denoted by the letter "G''.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{1432f7.ps} \end{figure}$	Figure 7: Top: the slope of the projected mass density profile plotted against H₀ for 121 different non-parametric models. Bottom: probability distribution of the derived H₀ values for the same models as above. The median value of the distribution is indicated by the dotted line.
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