All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{9716fig1.eps}\end{figure}$ Figure 1: The variability Doppler factors $D_{\rm var}$ plotted against thesynchrotron peak frequency. The $\nu '_{\rm p}$ -values are D-corrected.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9716fig2.eps}\end{figure}$ Figure 2: The peak luminosity of the synchrotron component plotted versus the synchrotron peak frequency. In the top panel, the values are z-corrected, and in the bottom panel Doppler-corrected. AGN classes are marked with different symbols (see legend).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9716fig3.eps}\end{figure}$ Figure 3: The Doppler-corrected synchrotron peak luminosity vs. peakfrequency correlation for bona fide blazars.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9716fig4.eps}\end{figure}$ Figure 4: Synchrotron peak luminosity versus peak frequency correlation for BLOs. The data are combined from this work (open circles) and Paper I (filled circles). The former are D-corrected, the latter are only z-corrected (i.e., we assume that they are not Doppler-boosted). In the top panel, the datapoints represented by open circles are D³-corrected, in the bottom panel they are D²-corrected. See text for details.
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In the text

$\begin{figure} \par {\includegraphics[width=16cm,clip]{9716fi5a.eps} } \end{figure}$ Figure 5: The spectral energy distributions determined in this work. All quantities are observational and uncorrected for redshift and Doppler boosting. The dashed line represents the parabolic fit to the synchrotron component. Datapoints marked with filled circles are included in the fit, the empty squares are not. Sources 1019+222 and 1845+797 could not be fitted with a parabolic function.
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In the text

$\begin{figure}{\includegraphics[width=16cm,clip]{9716fi5b.eps} } \end{figure}$ Figure 5: continued.
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In the text

$\begin{figure}{\includegraphics[width=16cm,clip]{9716fi5c.eps} } \end{figure}$ Figure 5: continued.
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In the text

$\begin{figure}{\includegraphics[width=16cm,clip]{9716fi5d.eps} } \end{figure}$ Figure 5: continued.
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In the text

$\begin{figure}{\includegraphics[width=16cm,clip]{9716fi5e.eps} } \end{figure}$ Figure 5: continued.
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In the text

$\begin{figure}{\includegraphics[width=16cm,clip]{9716fi5f.eps} } \end{figure}$ Figure 5: continued.
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In the text

$\begin{figure}{\includegraphics[width=16cm,clip]{9716fi5g.eps} } \end{figure}$ Figure 5: continued.
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In the text

$\begin{figure}{\includegraphics[width=16cm,clip]{9716fi5h.eps} } \end{figure}$ Figure 5: continued.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9716fig1.eps}\end{figure}$	Figure 1: The variability Doppler factors $D_{\rm var}$ plotted against thesynchrotron peak frequency. The $\nu '_{\rm p}$ -values are D-corrected.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9716fig2.eps}\end{figure}$	Figure 2: The peak luminosity of the synchrotron component plotted versus the synchrotron peak frequency. In the top panel, the values are z-corrected, and in the bottom panel Doppler-corrected. AGN classes are marked with different symbols (see legend).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9716fig3.eps}\end{figure}$	Figure 3: The Doppler-corrected synchrotron peak luminosity vs. peakfrequency correlation for bona fide blazars.
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$\begin{figure} \par {\includegraphics[width=16cm,clip]{9716fi5a.eps} } \end{figure}$	Figure 5: The spectral energy distributions determined in this work. All quantities are observational and uncorrected for redshift and Doppler boosting. The dashed line represents the parabolic fit to the synchrotron component. Datapoints marked with filled circles are included in the fit, the empty squares are not. Sources 1019+222 and 1845+797 could not be fitted with a parabolic function.
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$\begin{figure}{\includegraphics[width=16cm,clip]{9716fi5b.eps} } \end{figure}$	Figure 5: continued.
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