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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2233fig1.eps}\end{figure}$ Figure 1: The outline of the two-level iteration process.
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In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{2233fig2.eps}\end{figure}$ Figure 2: The finite differencing coefficients for $\kappa$ ( left), $\gamma _1$ ( middle) and $\gamma _2$ ( right). E.g. for $\kappa$ we use a formula including 9 points, the multiplicative factor is given at the bottom, the individual coefficients in the circle. Thus for the middle point (0,0) we get $\kappa(0,0) = \frac{1}{2}\frac{1}{6\Delta} \left[ 2\left\lbrack \psi(-1,1) + ... ...(0,1) + \psi(-1,0) + \psi(1,0) + \psi(0,-1) \right\rbrack - 4 \psi(0,0)\right]$ .
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In the text

$\begin{figure} \par\includegraphics[width=4.3cm,clip]{2233fig3.eps}\end{figure}$ Figure 3: The intrinsic invariance of the method. If we alternately add/subtract a constant a along the diagonals the shear $\gamma$ does not change (cf. Fig. 2), but $\kappa$ changes in the similar way with a constant now being 2a/3.
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In the text

$\begin{figure} \par\includegraphics[width=15.2cm]{2233fig4.ps}\par {\hspace*{4cm} \bf (a)\hspace*{7.5cm} \bf (b)\hspace*{4cm}} \par\end{figure}$ Figure 4: The gravitational lensing properties of a simulated cluster used for generating mock catalogues for statistical weak lensing and for the multiple image system. a) The surface mass density $\kappa$ ; b) the absolute value of the reduced shear $\left\vert g \right\vert$ , both for a source at $z_{\rm s} \to \infty$ , are given in gray-scale and contours. The stars in a) denote the image positions of a four-image system at $z_{\rm s} = 1.76$ which we use for the reconstruction.
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In the text

$\begin{figure} \par\subfigure[{\bf (a1)}]{\includegraphics[width=6cm,clip]{2233f... ...figure[{\bf (c2)}]{\includegraphics[width=6cm,clip]{2233fig5f.ps} } \end{figure}$ Figure 5: $\kappa$ -maps obtained from combined strong and weak lensing reconstruction of the simulated data. Left panels show the reconstructions using $N_{\rm g} = 210$ galaxies distributed in the same manner as the I-band, while for the right panels we use $N_{\rm g} = 148$ galaxies distributed in the same manner as the R-band weak lensing data for RX J1347.5-1145 (see Paper II). The galaxies have been lensed by an N-body simulated cluster. Different initial conditions are used for the reconstruction. In a1)- a2) we use best fit model from the multiple image system IM (see Sect. 4.2) in b1)- b2) we use the IC model, an NIS model with the same scaling and core radius as IM and in c1)- c2) we use I0, i.e. $\kappa ^{(0)}=0$ on all grid points. The positions of the cluster centre and two major subclumps are plotted as white circles.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2233fig1.eps}\end{figure}$	Figure 1: The outline of the two-level iteration process.
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$\begin{figure} \par\includegraphics[width=4.3cm,clip]{2233fig3.eps}\end{figure}$	Figure 3: The intrinsic invariance of the method. If we alternately add/subtract a constant a along the diagonals the shear $\gamma$ does not change (cf. Fig. 2), but $\kappa$ changes in the similar way with a constant now being 2a/3.
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