All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig1.ps} \end{figure}$ Figure 1: 0108+388 at 1.36 GHz. 0.4 Jy has been subtracted at the core position to improve the detection of extended emission close to the compact component.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig2.ps} \end{figure}$ Figure 2: 0237-233 at 1.66 GHz.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig3.ps} \end{figure}$ Figure 3: Radio contours of 0248+430 at 1.36 GHz superimposed to the gray scale POSS2 image.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig4.ps} \end{figure}$ Figure 4: Radio contours of 0316+162 at 1.36 GHz superimposed to the gray scale POSS2 image.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig5.ps} \end{figure}$ Figure 5: 0500+019 at 1.36 GHz.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig6.ps} \end{figure}$ Figure 6: 0743-006 at 1.36 GHz.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig7.ps} \end{figure}$ Figure 7: Radio contours of 0941-080 at 1.36 GHz superimposed to the NOT optical image (gray scale and thinner contours). First radio contour is 0.5 mJy. Peak in the radio image is 2.726 Jy.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig8.ps} \end{figure}$ Figure 8: Radio contours of 1127-145 at 1.36 GHz superimposed to the gray scale POSS2 image.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{2226fig9.ps} \end{figure}$ Figure 9: 1127-145 from mas to arcsecond scale.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{2226fi10.ps} \end{figure}$ Figure 10: Radio contours of 1245-197 at 1.36 GHz superimposed to the gray scale POSS2 image.
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In the text

$\begin{figure} \par\includegraphics[width=13.2cm,clip]{2226fi11.ps}\end{figure}$ Figure 11: Radio contours of 1345+125 superimposed to the NOT optical image (gray scale image and thinner contours). First radio contour is 1 mJy. The peak in the image is 64.8 mJy. A point like component of 5.2 Jy has been subtracted at the peak position to enhance the visibility of the diffuse emission around the core.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{2226fi12.ps}\end{figure}$ Figure 12: Radio contours of 1404+286 at 1.36 GHz superimposed to the gray scale POSS2 image
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2226f13a.ps}\hspace*{4mm} \includegraphics[width=7.8cm,clip]{2226f13b.ps}\end{figure}$ Figure 13: 1518+047 from the FIRST ( left) and from present data ( right).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2226f14a.ps}\hspace*{4mm} \includegraphics[width=7.8cm,clip]{2226f14b.ps}\end{figure}$ Figure 14: 2008-068 from the FIRST ( left) and from present data ( right).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fi15.ps}\end{figure}$ Figure 15: Radio image of 2128+048 at 1.36 GHz.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{2226fi16.ps}\end{figure}$ Figure 16: 2134+004 at mas ( left) and arcsecond resolution ( right). In the VLA image most of the core flux density has been subtracted to enhance the visibility of the diffuse emission.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{2226fi17.ps}\end{figure}$ Figure 17: The effect of redshift on extended emission detectability. Left image is 0738+313 at z=0.631, center image is how it would appear at z=2, right image is how it would appear at z=3. The dependence of angular size with redshift has not been taken into consideration because at these high redshifts angular size does not depend strongly on redshift.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm]{2226fi18.eps}\end{figure}$ Figure 18: Flux density at 1.36 GHz of extended emission versus redshift. Continuous lines approximately separate regions of FRI and FRII radio sources, filled circles are quasars, empty circle are galaxies, thick arrows are higher limits for quasars, thin arrows are higher limits for galaxies (see Sect. 4).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig1.ps} \end{figure}$	Figure 1: 0108+388 at 1.36 GHz. 0.4 Jy has been subtracted at the core position to improve the detection of extended emission close to the compact component.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig2.ps} \end{figure}$	Figure 2: 0237-233 at 1.66 GHz.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig3.ps} \end{figure}$	Figure 3: Radio contours of 0248+430 at 1.36 GHz superimposed to the gray scale POSS2 image.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig4.ps} \end{figure}$	Figure 4: Radio contours of 0316+162 at 1.36 GHz superimposed to the gray scale POSS2 image.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig5.ps} \end{figure}$	Figure 5: 0500+019 at 1.36 GHz.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig6.ps} \end{figure}$	Figure 6: 0743-006 at 1.36 GHz.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig7.ps} \end{figure}$	Figure 7: Radio contours of 0941-080 at 1.36 GHz superimposed to the NOT optical image (gray scale and thinner contours). First radio contour is 0.5 mJy. Peak in the radio image is 2.726 Jy.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fig8.ps} \end{figure}$	Figure 8: Radio contours of 1127-145 at 1.36 GHz superimposed to the gray scale POSS2 image.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{2226fig9.ps} \end{figure}$	Figure 9: 1127-145 from mas to arcsecond scale.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{2226fi10.ps} \end{figure}$	Figure 10: Radio contours of 1245-197 at 1.36 GHz superimposed to the gray scale POSS2 image.
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$\begin{figure} \par\includegraphics[width=13.2cm,clip]{2226fi11.ps}\end{figure}$	Figure 11: Radio contours of 1345+125 superimposed to the NOT optical image (gray scale image and thinner contours). First radio contour is 1 mJy. The peak in the image is 64.8 mJy. A point like component of 5.2 Jy has been subtracted at the peak position to enhance the visibility of the diffuse emission around the core.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{2226fi12.ps}\end{figure}$	Figure 12: Radio contours of 1404+286 at 1.36 GHz superimposed to the gray scale POSS2 image
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2226f13a.ps}\hspace*{4mm} \includegraphics[width=7.8cm,clip]{2226f13b.ps}\end{figure}$	Figure 13: 1518+047 from the FIRST ( left) and from present data ( right).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2226f14a.ps}\hspace*{4mm} \includegraphics[width=7.8cm,clip]{2226f14b.ps}\end{figure}$	Figure 14: 2008-068 from the FIRST ( left) and from present data ( right).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2226fi15.ps}\end{figure}$	Figure 15: Radio image of 2128+048 at 1.36 GHz.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{2226fi16.ps}\end{figure}$	Figure 16: 2134+004 at mas ( left) and arcsecond resolution ( right). In the VLA image most of the core flux density has been subtracted to enhance the visibility of the diffuse emission.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{2226fi17.ps}\end{figure}$	Figure 17: The effect of redshift on extended emission detectability. Left image is 0738+313 at z=0.631, center image is how it would appear at z=2, right image is how it would appear at z=3. The dependence of angular size with redshift has not been taken into consideration because at these high redshifts angular size does not depend strongly on redshift.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm]{2226fi18.eps}\end{figure}$	Figure 18: Flux density at 1.36 GHz of extended emission versus redshift. Continuous lines approximately separate regions of FRI and FRII radio sources, filled circles are quasars, empty circle are galaxies, thick arrows are higher limits for quasars, thin arrows are higher limits for galaxies (see Sect. 4).
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