$\begin{figure} \par\includegraphics[width=5.5cm,clip]{5266fig1.eps}\end{figure}$ Figure 1: Open circles correspond to FRIs and stars to FRIIs, with filled symbols for high-excitation emission line galaxies. The solid line marks the Ledlow-Owen relation.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{5266fig2.eps}\end{figure}$ Figure 2: Examples of radio galaxy spectra with best-fit models overplotted as solid lines where an acceptable fit could be obtained. The K1 star used as a template for the fitting is shown at the top of each panel.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{5266fig3.eps}\end{figure}$ Figure 3: Comparison of red and blue velocity dispersions. Error bars represent 95% confidence intervals.
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In the text

$\begin{figure} \par\includegraphics[width=5.55cm,clip]{5266fig4.eps}\end{figure}$ Figure 4: Results from simulations with artificial galaxy spectra. The input velocity dispersions, $\sigma _{\rm in}$ , are recovered ( $\sigma _{\rm out}$ ) to within 10%.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{5266fig6.eps}\end{figure}$ Figure 6: From left to right, jet power, photoionizing luminosity and their ratio as a function of BH mass. An uncertainty of $\pm$ 1 dex in $Q_{\rm jet}$ and $Q_{\rm phot}$ has been assumed, and the 95% confidence interval on BH mass is used. Symbols are as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{5266fig1.eps}\end{figure}$	Figure 1: Open circles correspond to FRIs and stars to FRIIs, with filled symbols for high-excitation emission line galaxies. The solid line marks the Ledlow-Owen relation.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16cm,clip]{5266fig2.eps}\end{figure}$	Figure 2: Examples of radio galaxy spectra with best-fit models overplotted as solid lines where an acceptable fit could be obtained. The K1 star used as a template for the fitting is shown at the top of each panel.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{5266fig3.eps}\end{figure}$	Figure 3: Comparison of red and blue velocity dispersions. Error bars represent 95% confidence intervals.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=5.55cm,clip]{5266fig4.eps}\end{figure}$	Figure 4: Results from simulations with artificial galaxy spectra. The input velocity dispersions, $\sigma _{\rm in}$ , are recovered ( $\sigma _{\rm out}$ ) to within 10%.
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$\begin{figure} \par\includegraphics[width=5.55cm,clip]{5266fig5.eps}\end{figure}$	Figure 5: Comparison with dispersions from the literature.
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$\begin{figure} \par\includegraphics[width=15.9cm,clip]{5266fig6.eps}\end{figure}$	Figure 6: From left to right, jet power, photoionizing luminosity and their ratio as a function of BH mass. An uncertainty of $\pm$ 1 dex in $Q_{\rm jet}$ and $Q_{\rm phot}$ has been assumed, and the 95% confidence interval on BH mass is used. Symbols are as in Fig. 1.
Open with DEXTER