Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{4611_f1.eps}\hspace*{4mm} \includegraphics[width=7cm,clip]{4611_f2.eps} \end{figure}$ Figure 1: The luminosity of the optical nuclei $L_{\rm o}$ , plotted against the radio core prominence $R_{\rm c}$ , for the FRI ( left) and FRII radio galaxies ( right). $\bullet$ radio galaxies, $\star$ BLRGs, $\downarrow$ and $\leftarrow$ upper limits. Statistics for the fits are listed in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4611_f3.eps}\hspace*{4mm} \includegraphics[width=7.1cm,clip]{4611_f4.eps} \end{figure}$ Figure 2: Nuclear optical luminosity $L_{\rm o}$ ( left) and radio core prominence $R_{\rm c}$ ( right) plotted against minor-to-major axis ratio b/a, for the FRI radio galaxies. $\bullet$ and $\blacksquare$ denote the dust disks and lanes respectively, from Verdoes Kleijn et al. (1999) while the open stars and $\blacktriangle$ denote the dust disks and lanes from de Koff et al. (2000), $\downarrow$ upper limits. The sources common to the two papers are shown by an open star superimposed by $\bullet$ . Table 1 lists the statistics for the correlations.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4611_f5.eps}\hspace*{4mm} \includegraphics[width=7cm,clip]{4611_f6.eps} \end{figure}$ Figure 3: Nuclear optical luminosity $L_{\rm o}$ versus radio core prominence $R_{\rm c}$ for the FRI population ( left): $\bullet$ radio galaxies, $\blacktriangledown$ BL Lac objects. $L_{\rm o}$ vs. $R_{\rm c}$ for the FRII population ( right): $\bullet$ radio galaxies, $\blacktriangledown$ radio-loud quasars, $\star$ BLRGs. $\downarrow$ and $\leftarrow$ upper limits, $\rightarrow$ lower limits. Statistics for the fits are listed in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4611_f7.eps}\hspace*{4mm} \includegraphics[width=7cm,clip]{4611_f8.eps} \end{figure}$ Figure 4: Nuclear optical luminosity $L_{\rm o}$ versus radio core prominence $R_{\rm c}$ for the matched subsample of FRI galaxies and BL Lac objects ( left) and FRII galaxies and quasars ( right). $\bullet$ radio galaxies, $\blacktriangledown$ BL Lac objects ( left) and quasars ( right), $\star$ BLRGs, $\downarrow$ upper limits, $\rightarrow$ lower limits. Statistics for the fits are listed in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4611_f11.eps}\hspace*{4mm} \includegraphics[width=7.5cm,clip]{4611_f12.eps} \end{figure}$ Figure 6: AIC values for different initial A_V₀ plotted against torus opening angles $\theta _{\rm c}$ (in degrees) for the FRI ( left) and the FRII ( right) populations for the "Jet+Torus'' model. For a given A_V₀, AIC was estimated at 2 $\hbox {$^\circ $ }$ intervals of $\theta _{\rm c}$ . The shaded area denotes the region where the model becomes unphysical (see Sect. 3.5.1). In the physical regime, AIC reaches a minimum at around 90 $\hbox {$^\circ $ }$ for the FRIs and 37 $\hbox {$^\circ $ }$ for the FRIIs.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{4611_f13.eps}\hspace*{4mm} \includegraphics[width=7.2cm,clip]{4611_f14.eps} \end{figure}$ Figure 7: AIC values for different initial A_V₀ plotted against torus opening angles $\theta _{\rm c}$ (in degrees) for the matched subsamples of FRI ( left) and the FRII ( right) populations for the "Jet+Torus'' model. The shaded area denotes the region where the model becomes unphysical (see Sect. 3.5.1). In the physical regime, AIC reaches a minimum at around 90 $\hbox {$^\circ $ }$ for the FRIs while the case is not clear for the FRIIs.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{4611_f1.eps}\hspace*{4mm} \includegraphics[width=7cm,clip]{4611_f2.eps} \end{figure}$	Figure 1: The luminosity of the optical nuclei $L_{\rm o}$ , plotted against the radio core prominence $R_{\rm c}$ , for the FRI ( left) and FRII radio galaxies ( right). $\bullet$ radio galaxies, $\star$ BLRGs, $\downarrow$ and $\leftarrow$ upper limits. Statistics for the fits are listed in Table 1.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4611_f9.eps}\hspace*{4mm} \includegraphics[width=7.5cm,clip]{4611_f10.eps} \end{figure}$	Figure 5: Best fits to the FRI ( left) and FRII ( right) populations using only a "Jet+Torus'' model. Table 2 lists the model parameters.
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