All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=15cm,clip]{fig1.ps}\end{figure}$ Figure 1: Distribution of redshift, M_R(host), and M_R(QSO) for the present sample.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{fig2a.ps}\vglue 0.5cm \includegraphics[angle=-90,width=8cm,clip]{fig2b.ps}\end{figure}$ Figure 2: The distribution of a) $\Lambda$ and b) $\lambda$ . The solid histograms plot the FSRQs, and the dotted-dashed histograms show the SSRQs. The dotted histograms show the total distribution for all RLQs (FSRQs and SSRQs). The distribution of $\lambda$ is divided into four regions, corresponding to different states of the accretion disks: (1) $\lambda < \lambda _1$ (pure ADAF); (2) $\lambda _1 \le \lambda \le \lambda _2$ (ADAF+SS); (3) $\lambda _2 \le \lambda \le \lambda _3$ (SS); (4) $\lambda \ge \lambda _3$ (SEA).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16.5cm,clip]{fig3.ps}\end{figure}$ Figure 3: The distribution of extended radio power at 5 GHz versus the a) $\lambda$ , b) $\Lambda$ , and c) $M_{\rm BH}$ . The filled circles show the FSRQs, and SSRQs are denoted as open stars. The open and semi-filled circles represent high frequency-peaked and low frequency-peaked BL Lacs, respectively; the radio data for these objects are taken from Urry et al. (2000), and values for $\lambda$ , $\Lambda$ , and $M_{\rm BH}$ are taken from Wang et al. (2002). The diagonal line in panel c) is the empirical division between FR I and FR II radio galaxies in the diagram of extended radio power at 1.4 GHz versus optical R-band absolute magnitude, as presented by Ledlow & Owen (1996); see text for details.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15cm,clip]{fig1.ps}\end{figure}$	Figure 1: Distribution of redshift, M_R(host), and M_R(QSO) for the present sample.
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