All Figures

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{H4340f1.eps} \end{figure}$ Figure 1: Redshifts and apparent V magnitudes of the sample quasars. Radio-quiet quasars are marked by crosses, flat spectrum radio-loud quasars and steep spectrum radio-loud quasars by open squares and filled squares respectively. Non-classified radio-loud quasars are marked with a triangle.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4340f2.ps} \end{figure}$ Figure 2: Position of the filter profiles at z = 0.5 and z=0.8. We use template galaxy spectra from Kinney et al. (1996) and the composite quasar spectrum from Vanden Berk et al. (2001). The intensity scales are arbitrary.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{H4340f3.ps} \end{figure}$ Figure 3: Contour plots of the quasar KUV 0200-0858. To the left the residual after subtraction of the empirical PSF and to the right after subtraction of the combined PSF. North is up, east to the left. The contours mark the 21, 22, 23, 24 and 25 mag arcsec^-2 levels and the image scale is in arcseconds.
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In the text

$\begin{figure} \par\includegraphics[width=10cm,clip]{H4340f4.eps} \end{figure}$ Figure 4: The distribution of host galaxy R magnitudes with redshift. No marginally resolved objects have been included in the plot. Open squares mark flat spectrum radio-loud objects, filled squares steep spectrum radio-loud objects and triangles non-classified radio-loud objects. Radio-quiet objects are marked with crosses. The solid line is the Hubble R-z relation for radio galaxies (O'Dea et al. 1996). The long-dashed line shows the apparent magnitude of an L^* galaxy calculated using the K-correction from Fukugita et al. (1995) for an E galaxy. For the short-dashed line the Sbc galaxy type K-correction was used, while for the dash-dotted line the Im type K-correction was applied. The typical $2\sigma$ error in the host galaxy magnitudes is represented by the bar in the lower right corner.
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In the text

$\begin{figure} \par\includegraphics[width=10cm,clip]{H4340f5.eps} \end{figure}$ Figure 5: The distribution with redshift of host galaxy R magnitudes from the literature. The lines are the same as in Fig. 4. Shown here is the (R96) NTT data (symbols for radio-quiet, FS and SS radio-loud objects as in Fig. 4) and samples from Hooper et al. (1997), Márquez et al. (1999), Kotilainen et al. (1998) and Kotilainen & Falomo (2000), marked as indicated in the figure. Only resolved objects have been plotted.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f6a.eps} \end{figure}$ Figure A.1: For each object field we present the luminosity profile in mag arcsec^-2 with radius in arcsec (points: quasar profile, full-drawn line: PSF, dotted line: residual); centered greyscale images of residual (top left), unsubtracted quasar (top right) and test star remainder (bottom right); contour plot of the residual (number inside frame is lowest contour level in mag arcsec^-2, spacing of contours is 1 mag arcsec^-2). The image sizes are 12 $.\!\!^{\prime\prime}$ 5 to a side, except for EX 0240+0044, where it is $20\hbox {$^{\prime \prime }$ }\times 20\hbox {$^{\prime \prime }$ }$ . North is up and east is to the left.

In the text

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{H4340f6b.eps}\end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7a.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7b.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7c.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7d.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7e.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7f.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7g.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7h.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7i.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7j.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7k.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7l.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7m.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4340f7n.eps} \end{figure}$ Figure A.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{H4340f1.eps} \end{figure}$	Figure 1: Redshifts and apparent V magnitudes of the sample quasars. Radio-quiet quasars are marked by crosses, flat spectrum radio-loud quasars and steep spectrum radio-loud quasars by open squares and filled squares respectively. Non-classified radio-loud quasars are marked with a triangle.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4340f2.ps} \end{figure}$	Figure 2: Position of the filter profiles at z = 0.5 and z=0.8. We use template galaxy spectra from Kinney et al. (1996) and the composite quasar spectrum from Vanden Berk et al. (2001). The intensity scales are arbitrary.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{H4340f3.ps} \end{figure}$	Figure 3: Contour plots of the quasar KUV 0200-0858. To the left the residual after subtraction of the empirical PSF and to the right after subtraction of the combined PSF. North is up, east to the left. The contours mark the 21, 22, 23, 24 and 25 mag arcsec^-2 levels and the image scale is in arcseconds.
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