All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{0676.f1}\end{figure}$ Figure 1: a) Integrated fraction of sources with total radio power at 1.4 GHz below $P_{\rm t}$ . Continuous and dotted-dashed lines stand for FR I and FR II type radio galaxies, respectively. The vertical dotted line represents the break power between FR I and FR II radio galaxies. b) Integrated fraction of sources with core radio power at 4.9 GHz below $P_{\rm c}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0676.f2}\end{figure}$ Figure 2: Distribution of redshift in our sample for FR I ( top) and FR II ( bottom) radio galaxies. The redshift bin is 0.025.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0676.f3}\par\end{figure}$ Figure 3: Distribution of the arm-length ratio for FR I ( top) and FR II ( bottom) radio galaxies. The filled circles and lines represent the prediction of an orientation-based model considering the jet-head advance velocity Gaussian distribution plotted in the small frame.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0676.f4}\par\end{figure}$ Figure 4: Total power at 1.4 GHz vs. core power at 4.9 GHz. The continuous line represents a least squares fit to our data. The dotted line represents the correlation $\log P_{\rm c}(4.9~\rm GHz) = (0.62\pm 0.04)$ $\log~ P_{\rm t}(0.408~\rm GHz) + (7.6\pm 1.1)$ by Giovannini et al. (2001) transformed to $P_{\rm t}$ (1.4 GHz), assuming an spectral index $\alpha =-0.75$ . Filled and empty circles correspond to FR I and FR II type radio galaxies, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0676.f5}\end{figure}$ Figure 5: Distribution of the orientation indicator R (see text) in logarithmic scales, for FR Is ( top) and FR IIs ( bottom) radio galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0676.f6}\par\end{figure}$ Figure 6: Distribution of the orientation indicator $P_{\rm CN}$ (see text) in logarithmic scales, for the whole sample ( top), FR Is ( middle) and FR IIs ( bottom) radio galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0676.f7}\par\end{figure}$ Figure 7: Distribution of parameter $P_{\rm CN}$ in logarithmic scales for sources with projected linear sizes smaller ( top) and larger ( bottom) than 1 Mpc.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0676.f8}\par\end{figure}$ Figure 8: Orientation indicator $P_{\rm CN}$ as a function of linear size. Symbols represent the same as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0676.f9}\par\end{figure}$ Figure 9: Apparent correlation between the core radio power and the source linear size, induced by the sample biases. The dashed line represents the influence of the selection criteria and of the $P_{\rm c}$ (4.9) vs. $P_{\rm t}$ (1.4) correlation in this plot. Symbols represent the same as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0676.f10}\par\end{figure}$ Figure 10: Distribution of the effective radius of the host galaxies observed at optical wavelengths (Paper II).
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{0676.f11}\par\end{figure}$ Figure 11: Power-size diagram of radio galaxies. Filled circles correspond to our sample; crosses correspond to the B2 sample; x-shaped crosses correspond to a compilation of GRGs (Ishwara-Chandra & Saikia 1999; Schoenmakers et al. 2000a; Machalski et al. 2001); asterisks correspond to the Peacock & Wall (1981) sample. The dashed line represents the sensitivity limit of the NVSS for a 16' extended 100 mJy source (see Paper I). The horizontal dotted line marks the power break between FR I and FR II radio sources. The vertical dotted line marks the definition of GRGs. The curved continuous lines represent evolutionary tracks for sources with jet powers of ( top to bottom) $1.3\times 10^{40}$ , $1.3\times 10^{39}$ and $1.3\times 10^{38}$ W from Kaiser et al. (1997). The straight continuous line represents the trend imposed by our selection criteria in flux density and source angular size.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0676.f12}\par\end{figure}$ Figure 12: Distribution of redshift of giant radio galaxies. The white histogram corresponds to a compilation of 115 GRGs (see text for references). The black histogram corresponds to the GRGs in our sample.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0676.f13}\end{figure}$ Figure 13: Relative number of FR I and FR II type radio galaxies as a function of redshift. The continuous line represents the result obtained from our sample. The dashed line is the result obtained from the Dunlop & Peacock (1990) RLF.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0676.f14}\par\end{figure}$ Figure 14: a) Number of radio sources with flux density at 1.4 GHz above 100 mJy and angular size above 4' per redshift bin of 0.05 obtained from our sample (asterisks). The continuous line represents the number of sources with flux density above 100 mJy at 1.4 GHz and unconstrained angular size obtained from the Dunlop & Peacock RLF. b) Filled dots represent the same as asterisks in a), but only considering FR I type radio galaxies. The continuous line represents the number of FR I type radio galaxies from the RLF, scaled by a factor of 0.047. c) Same as b), but for FR II type radio galaxies. The continuous line results from the RLF after applying a scaling factor of 0.22.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0676.f1}\end{figure}$	Figure 1: a) Integrated fraction of sources with total radio power at 1.4 GHz below $P_{\rm t}$ . Continuous and dotted-dashed lines stand for FR I and FR II type radio galaxies, respectively. The vertical dotted line represents the break power between FR I and FR II radio galaxies. b) Integrated fraction of sources with core radio power at 4.9 GHz below $P_{\rm c}$ .
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0676.f2}\end{figure}$	Figure 2: Distribution of redshift in our sample for FR I ( top) and FR II ( bottom) radio galaxies. The redshift bin is 0.025.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0676.f3}\par\end{figure}$	Figure 3: Distribution of the arm-length ratio for FR I ( top) and FR II ( bottom) radio galaxies. The filled circles and lines represent the prediction of an orientation-based model considering the jet-head advance velocity Gaussian distribution plotted in the small frame.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0676.f5}\end{figure}$	Figure 5: Distribution of the orientation indicator R (see text) in logarithmic scales, for FR Is ( top) and FR IIs ( bottom) radio galaxies.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0676.f6}\par\end{figure}$	Figure 6: Distribution of the orientation indicator $P_{\rm CN}$ (see text) in logarithmic scales, for the whole sample ( top), FR Is ( middle) and FR IIs ( bottom) radio galaxies.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0676.f7}\par\end{figure}$	Figure 7: Distribution of parameter $P_{\rm CN}$ in logarithmic scales for sources with projected linear sizes smaller ( top) and larger ( bottom) than 1 Mpc.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0676.f8}\par\end{figure}$	Figure 8: Orientation indicator $P_{\rm CN}$ as a function of linear size. Symbols represent the same as in Fig. 4.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0676.f9}\par\end{figure}$	Figure 9: Apparent correlation between the core radio power and the source linear size, induced by the sample biases. The dashed line represents the influence of the selection criteria and of the $P_{\rm c}$ (4.9) vs. $P_{\rm t}$ (1.4) correlation in this plot. Symbols represent the same as in Fig. 4.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0676.f10}\par\end{figure}$	Figure 10: Distribution of the effective radius of the host galaxies observed at optical wavelengths (Paper II).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0676.f12}\par\end{figure}$	Figure 12: Distribution of redshift of giant radio galaxies. The white histogram corresponds to a compilation of 115 GRGs (see text for references). The black histogram corresponds to the GRGs in our sample.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0676.f13}\end{figure}$	Figure 13: Relative number of FR I and FR II type radio galaxies as a function of redshift. The continuous line represents the result obtained from our sample. The dashed line is the result obtained from the Dunlop & Peacock (1990) RLF.
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