All Figures

$\begin{figure} \par\includegraphics[width=8cm]{0303fig1.ps} %\end{figure}$ Figure 1: HST image of the host galaxy of 3C 313 (in the center). The size of the image is $4\times4~{\rm arcsec^2}$ . The nucleus of this source has a complex morphology (see discussion in the text, Sect. 4).
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In the text

$\begin{figure} \includegraphics[width=8cm,clip]{0303fig2.ps} \end{figure}$ Figure 2: Optical luminosity of the CCC vs. radio core luminosity. The two shaded regions represent the positions of the FR I sample and the sample of FR II at z<0.3.
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In the text

$\begin{figure} \includegraphics[width=8cm,clip]{0303fig3.ps} \end{figure}$ Figure 3: Same as Fig. 2; enlargement of the range of luminosities of the present sample. Different symbols refer to different spectral classifications. The empty circle corresponds to the only unclassified source (namely 3C 435A).
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In the text

$\begin{figure} \includegraphics[width=7cm,clip]{0303fig4.ps} \end{figure}$ Figure 4: Equivalent Width of the [OIII] emission line, measured with respect to the CCC emission, plotted vs. the ratio between the optical CCC to radio core flux. The shaded area represents the dispersion ( $1\sigma$ ) of the linear correlation between radio core and CCC luminosity found for FR I in Paper I. The dashed horizontal line is the separation between "obscured'' and "unobscured'' sources (see text, Sect. 5.1).
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In the text

$\begin{figure} \includegraphics[width=17cm,clip]{0303fig5.ps} \end{figure}$ Figure 5: HST optical image of 3C 295 ( on the left) and residuals after the subtraction of the model obtained with a isophotal fitting ( on the right). The circle is the center of the galaxy model. The dimension of both boxes is $1.8\times1.8~{\rm arcsec^2}$ . See text for discussion (Sect. 5.1).
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{0303fig1.ps} %\end{figure}$	Figure 1: HST image of the host galaxy of 3C 313 (in the center). The size of the image is $4\times4~{\rm arcsec^2}$ . The nucleus of this source has a complex morphology (see discussion in the text, Sect. 4).
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$\begin{figure} \includegraphics[width=8cm,clip]{0303fig2.ps} \end{figure}$	Figure 2: Optical luminosity of the CCC vs. radio core luminosity. The two shaded regions represent the positions of the FR I sample and the sample of FR II at z<0.3.
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$\begin{figure} \includegraphics[width=8cm,clip]{0303fig3.ps} \end{figure}$	Figure 3: Same as Fig. 2; enlargement of the range of luminosities of the present sample. Different symbols refer to different spectral classifications. The empty circle corresponds to the only unclassified source (namely 3C 435A).
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$\begin{figure} \includegraphics[width=17cm,clip]{0303fig5.ps} \end{figure}$	Figure 5: HST optical image of 3C 295 ( on the left) and residuals after the subtraction of the model obtained with a isophotal fitting ( on the right). The circle is the center of the galaxy model. The dimension of both boxes is $1.8\times1.8~{\rm arcsec^2}$ . See text for discussion (Sect. 5.1).
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