$\begin{figure} \addtocounter{figure}{+1} \par\includegraphics[width=7cm,clip]{3945fg57.eps} \end{figure}$ Figure 2: Comparison between the VLA 15 GHz integrate flux densities and those extrapolated from the data in Paper I. The line has a slope of one.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3945fg58.eps} \end{figure}$ Figure 3: Core dominance distribution for the B3-VLA sources (filled circles) and 3CR sources (open circles).
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{3945fg59.eps} \includegraphics[width=6.8cm,clip]{3945fg60.eps} \end{figure}$ Figure 4: a) Top: distribution of $S{_{\rm R}}$ for LLS< 9 kpc ( $+45\hbox {$^\circ $ }$ shaded) and $LLS\geq$ 9 kpc ( $-45\hbox {$^\circ $ }$ shaded). The last bin includes the five sources (0039+398, 0123+402, 0809+404, 1044+454, 1136+420) with $S_{\rm R}>10$ . b) Bottom: $S{_{\rm R}}$ plotted as a function of LLS. Circles mark the sources with a (candidate) core; crosses are double sources. The broken curve roughly indicates the upper envelope of the distribution for $S_{\rm R}\leq 10$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3945fg61.eps} \end{figure}$ Figure 5: Flux density ratio ( $S{_{\rm R}}$ ) of the stronger to the weaker component vs. $d_{\rm R}^4$ . Filled and open triangles are sources with LLS<9 kpc and $LLS\geq 9$ kpc respectively.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{3945fg62.eps}\hspace*{2.2c... ...s}\hspace*{2.2cm} \includegraphics[width=6.7cm,clip]{3945fg65.eps} \end{figure}$ Figure 6: Spectral fit. The top panels refer to the source 0003+387, which results better fitted by a JP model. The bottom panels are the same for the source 1350+432, better fitted by a CI model.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3945fg66.eps}\hspace*{1.9cm} \includegraphics[width=7cm,clip]{3945fg67.eps} \end{figure}$ Figure 7: a) Left: injection spectral index distribution versus source linear size. Circles are for objects presented in this paper, squares for objects without the 15 GHz data (Zappacosta degree thesis). Filled symbols are for $\alpha _{\rm inj}$ obtained from a CI model and open ones from a JP model. There is no correlation. b) Right: source rest frame break frequency versus linear size. Symbols are as in a).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3945fg68.eps} \end{figure}$ Figure 8: Radiative ages distribution as function of the source linear size. Symbols are as in Fig. 7.
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In the text

$\begin{figure} \addtocounter{figure}{-8} \mbox{\includegraphics[width=8.4cm]{... ....eps} \hspace{4mm} \includegraphics[width=8.4cm]{3945fg02.eps} } \end{figure}$ Figure 1: VLA images. Thick contours: 15 GHz isophotes. First contour is three times the average rms noise level on the images (0.3 mJy/beam); contour levels increase by a factor of 2. Peak flux density is at 15 GHz. Thin contours: 8.5 GHz isophotes. First contour is three times the average rms noise level on the image (0.2 mJy/beam); contour levels increase by a factor of 8. The beams are almost circular with sizes $0\hbox{$.\!\!^{\prime\prime}$ }12\times 0\hbox{$.\!\!^{\prime\prime}$ }12$ .
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In the text

$\begin{figure} \addtocounter{figure}{+1} \par\includegraphics[width=7cm,clip]{3945fg57.eps} \end{figure}$	Figure 2: Comparison between the VLA 15 GHz integrate flux densities and those extrapolated from the data in Paper I. The line has a slope of one.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3945fg58.eps} \end{figure}$	Figure 3: Core dominance distribution for the B3-VLA sources (filled circles) and 3CR sources (open circles).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3945fg61.eps} \end{figure}$	Figure 5: Flux density ratio ( $S{_{\rm R}}$ ) of the stronger to the weaker component vs. $d_{\rm R}^4$ . Filled and open triangles are sources with LLS<9 kpc and $LLS\geq 9$ kpc respectively.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{3945fg62.eps}\hspace{2.2c... ...s}\hspace{2.2cm} \includegraphics[width=6.7cm,clip]{3945fg65.eps} \end{figure}$	Figure 6: Spectral fit. The top panels refer to the source 0003+387, which results better fitted by a JP model. The bottom panels are the same for the source 1350+432, better fitted by a CI model.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3945fg68.eps} \end{figure}$	Figure 8: Radiative ages distribution as function of the source linear size. Symbols are as in Fig. 7.
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$\begin{figure}\addtocounter{figure}{-1} \mbox{\includegraphics[width=8.4cm]{394... ...7.eps} \hspace{4mm} \includegraphics[width=8.4cm]{3945fg08.eps} } \end{figure}$	Figure 1: continued.
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