All Figures

$\begin{figure} \par\includegraphics[width=2.5cm,clip]{9712fig1.ps}\hspace*{1cm} ... ...ig7.ps}\hspace*{1cm} \includegraphics[width=2.5cm,clip]{9712fig8.ps}\end{figure}$ Figure 1: Images of all eight quasars in I. From upper left to lower right: FDF0809, FDF1837, FDF2229, FDF2633, FDF4683, FDF5962, FDF6007, FDF6233. Size of each picture is 20'' $\times$ 20'' respectively, pixelscale is 0 $.\!\!^{\prime\prime}$ 2/pixel, north is up, east is left.
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In the text

$\begin{figure} \par\includegraphics[width=13.9cm,clip]{9712fig9.eps}\end{figure}$ Figure 2: Fitting results of the resolved and marginally resolved objects, see text for discussion. From top to bottom: FDF0809 (ellipticity and PA fitted), FDF1837, FDF2229, FDF6007. Left panel: B band, right panel: I band. All intensities are plotted logarithmically and in arbitrary units. Radius in pixels.
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In the text

$\begin{figure} \par\includegraphics[width=13.9cm,clip]{9712fig10.eps}\end{figure}$ Figure 3: Fitting results of unresolved objects. From top to bottom: FDF2633, FDF4683, FDF5962, FDF6233. Left panel: B band, right panel: I band. All intensities are plotted logarithmically and in arbitrary units. Radius in pixels.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7cm,clip]{9712fig11.eps}\hspace*{1cm} \includegraphics[angle=270,width=7cm,clip]{9712fig12.eps} \end{figure}$ Figure 4: Simulation of the spectrum of FDF0809 in the I-band ( left) and B-band ( right). The solid line shows the measured spectrum in the restframe, the dashed lines show the simulated spectra (QSO+galaxy spectra added up) marked with the model type of the galaxy template. The wavelength range used for scaling is marked with dotted lines and the name of the corresponding filter. The Sb-model is unambiguously preferred in both cases.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.5cm,clip]{9712fig13.eps}\h... ...*{1cm} \includegraphics[angle=270,width=7.5cm,clip]{9712fig14.eps} \end{figure}$ Figure 5: Colours (B-I) of model galaxies as a function of redshift compared to the colours of our resolved galaxies. The redshift of the galaxy formation is z=3 ( left) and z=5 ( right) respectively. Filled triangles indicate the results of our fits with an elliptical galaxy and open triangles with a disk galaxy. The colours of burst galaxies are shown as dotted, the ones of long burst galaxies as long-dashed, the ones of E/S0 galaxies are shown as dash-dotted lines and the ones of Sb galaxies as solid lines, respectively. If a filter is influenced by forbidden or semi-forbidden lines, originating in the BLR/NLR the magnitude of the host galaxy in this filter can be overestimated, as the flux from these lines may be detected as host galaxy flux. This is indicated by arrows. Errors lie in the order of $\sim$ 1 mag.
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In the text

$\begin{figure} \par\includegraphics[width=2.5cm,clip]{9712fig1.ps}\hspace{1cm} ... ...ig7.ps}\hspace{1cm} \includegraphics[width=2.5cm,clip]{9712fig8.ps}\end{figure}$	Figure 1: Images of all eight quasars in I. From upper left to lower right: FDF0809, FDF1837, FDF2229, FDF2633, FDF4683, FDF5962, FDF6007, FDF6233. Size of each picture is 20'' $\times$ 20'' respectively, pixelscale is 0 $.\!\!^{\prime\prime}$ 2/pixel, north is up, east is left.
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$\begin{figure} \par\includegraphics[width=13.9cm,clip]{9712fig9.eps}\end{figure}$	Figure 2: Fitting results of the resolved and marginally resolved objects, see text for discussion. From top to bottom: FDF0809 (ellipticity and PA fitted), FDF1837, FDF2229, FDF6007. Left panel: B band, right panel: I band. All intensities are plotted logarithmically and in arbitrary units. Radius in pixels.
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$\begin{figure} \par\includegraphics[width=13.9cm,clip]{9712fig10.eps}\end{figure}$	Figure 3: Fitting results of unresolved objects. From top to bottom: FDF2633, FDF4683, FDF5962, FDF6233. Left panel: B band, right panel: I band. All intensities are plotted logarithmically and in arbitrary units. Radius in pixels.
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