All Figures

$\begin{figure} \par\mbox{\includegraphics[height=2.9cm,width=5.1cm,clip]{09434fi01.ps} \includegraphics[width=2.9cm,clip]{09434fi02.ps} } \end{figure}$ Figure 1: Left: color image of a small portion ( $\sim$ $1.1\hbox {$^\prime $ }$ $\times$ $\sim$ $0.7\hbox {$^\prime $ }$ ) of the northern subcluster created using the riz HST/ACS filters. The green circle on the top right, at a projected distance of 488 kpc and in direction $26.4\hbox {$^\circ $ }$ NE with respect to the centroid of the northern mass clump, which corresponds to two central galaxies (indicated by the red cross on the bottom left), shows the position of the strong lensing system considered in this paper. Right: zoom-in view of a $4\hbox {$^{\prime \prime }$ }$ $\times$ $4\hbox {$^{\prime \prime }$ }$ field around the lens galaxy at $z_{\rm l}=0.82$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{09434fi03.ps}\end{figure}$ Figure 2: Best four-image SIS+ES model. Top left: source plane with caustics. The predicted source position is indicated by the cross. The arrows display the directions of the northern cluster clump ( ${\rm\theta _{NC}}$ ), of the external shear predicted by the model ( ${\rm\theta _{\gamma }}$ ), of the galaxy ellipticity position angle (PA), and of the southern cluster clump ( ${\rm\theta _{SC}}$ ). Top right: image plane with critical curves. The observed (squares) and predicted (crosses) image positions are shown. Bottom left: contour levels of the Fermat potential. The images are two minima (A, C) and two saddle points (B, D). Bottom right: predicted deformation of the four images obtained by locating a small round source in the position illustrated on the top left panel.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{09434fi04.ps}\end{figure}$ Figure 3: Best twelve-image SIS+ES model. Left: source plane with caustics. The predicted components of the source are shown. Right: image plane with critical curves. The observed (squares) and predicted (triangles, crosses, and diamonds) images are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{09434fi05.ps}\end{figure}$ Figure 4: Results of the $\chi ^{2}$ minimizations of 200 Monte-Carlo generated data sets. Top: marginal distributions of the model parameters with their approximate normal distributions. Bottom: the joint density distributions show the parameter correlations.
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In the text

$\begin{figure} \par\includegraphics[width=4cm,clip]{09434fi06.ps}\includegraphic... ...cm,clip]{09434fi08.ps}\includegraphics[width=4cm,clip]{09434fi09.ps}\end{figure}$ Figure 5: Best extended-image SIS+ES model. Top left: the observed HST/ACS r field (5 $^{\prime \prime }$ across). Top right: the same image after the subtraction of an elliptical model fitted on the luminosity profile of the lens galaxy. Some residuals of the galaxy luminosity are still visible in the inner region. Bottom left: the best reconstruction of the lensed system. Bottom right: the residuals after the subtraction of the model predicted (third panel) from the observed (second panel) images. The central residuals due to the lens galaxy subtraction have been masked here.
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In the text

$\begin{figure} \par\includegraphics[width=4.85cm,clip]{09434fi10.ps}\end{figure}$ Figure 6: The source redshift obtained from gravitational lensing and stellar dynamics. The Einstein angle, from lensing analysis, and the velocity dispersion of the galaxy, from spectroscopic measurements, combine to give a lower limit for the redshift of the source. The dashed and dotted lines represent 1 and 2 $\sigma$ error bars, respectively. The vertical long-dashed line shows the spectroscopic upper limit of the source redshift discussed in Sect. 4.2.
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In the text

$\begin{figure} \par {\hspace*{2.05cm}\includegraphics[width=4.15cm,clip]{09434fi... ...space*{2.05cm}} \par\includegraphics[width=8.2cm,clip]{09434fi12.ps}\end{figure}$ Figure 7: Spectroscopic measurements of object A. Top: position of the 1 $^{\prime \prime }$ slit. Bottom: composite 2D sky-subtracted spectrum obtained with VLT/FORS2 in 5230 s. The arrow shows the Lyman alpha drop at 4730 $\AA$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{09434fi13.ps}\end{figure}$ Figure 8: The galaxy and cluster masses. Left: the lensing [ $M_{{\rm len}}(R \le 9.54~{\rm kpc})$ ] and dynamical [ $M_{{\rm dyn}}(R \le 9.54~{\rm kpc})$ ] measurements of the galaxy projected total mass inside a 9.54 kpc radius as a function of the source redshift. The dashed and dotted lines represent 1 and 2 $\sigma$ error bars, respectively. Right: the galaxy (dashed), the cluster (dotted), and the total (dashed-dotted) projected mass inside a 9.54 kpc radius centered on the galaxy. The long-dashed line shows the projected mass of the cluster inside a circle with a radius of 488 kpc, that is the distance between the cluster and the galaxy centers.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{09434fi14.ps}\end{figure}$ Figure 9: SED of the lens galaxy at $z_{\rm l}=0.82$ . The circles with the error bars represent, from left to right, the observed flux densities measured inside the 1.07 $^{\prime \prime }$ aperture in the HST/ACS (r, i, z) and NTT/SofI (J, Ks) passbands. The illustrated best-fit has been built with Bruzual & Charlot 2003 models. On the bottom, the best-fit values of the age (t), the characteristic time of the SFH ( ${\rm\tau }$ ), and the mass ( $M_{{\rm phot}}$ ) of the galaxy are given.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{09434fi04.ps}\end{figure}$	Figure 3: Best twelve-image SIS+ES model. Left: source plane with caustics. The predicted components of the source are shown. Right: image plane with critical curves. The observed (squares) and predicted (triangles, crosses, and diamonds) images are shown.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{09434fi05.ps}\end{figure}$	Figure 4: Results of the $\chi ^{2}$ minimizations of 200 Monte-Carlo generated data sets. Top: marginal distributions of the model parameters with their approximate normal distributions. Bottom: the joint density distributions show the parameter correlations.
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$\begin{figure} \par {\hspace{2.05cm}\includegraphics[width=4.15cm,clip]{09434fi... ...space{2.05cm}} \par\includegraphics[width=8.2cm,clip]{09434fi12.ps}\end{figure}$	Figure 7: Spectroscopic measurements of object A. Top: position of the 1 $^{\prime \prime }$ slit. Bottom: composite 2D sky-subtracted spectrum obtained with VLT/FORS2 in 5230 s. The arrow shows the Lyman alpha drop at 4730 $\AA$ .
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