All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0431f1.ps} \includegraphics[width=8.8cm,clip]{0431f2.ps} \end{figure}$ Figure 1: The estimate of the continuum (solid line) in the case of Mrk 1040 H $\beta$ (top) and H $\alpha$ (down). Dotted line the observed spectra and dashed line (below) the spectra after continuum subtraction.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0431f3.ps}\vspace*{1.4cm} \includegraphics[width=7.4cm,clip]{0431f4.ps} \end{figure}$ Figure 2: Decomposition of the H $\beta$ lines of the observed AGNs. The dashed lines represent the observations and the solid lines show the profile obtained by Gaussian decomposition. The Gaussian components are presented at the bottom. The dashed complex lines at the bottom represent the contribution of the Fe II, [OIII] and H $\beta$ narrow lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0431f5.ps} \end{figure}$ Figure 3: The estimated contribution of the H $\beta$ wing and other satellite lines in the [OIII] $\lambda \lambda 4959,5007$ line wavelength region (solid line) for Mrk 817.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0431f6.ps} \end{figure}$ Figure 4: Decomposition of the [OIII] lines.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0431f7.ps}\vspace*{1.4cm} \includegraphics[width=7.4cm,clip]{0431f8.ps} \end{figure}$ Figure 5: The same as in Fig. 2. but for the H $\alpha$ line. The narrow dashed lines at the bottom correspond to the narrow H $\alpha$ and [NII] lines, the broad dashed lines correspond to the Fe II and He I contribution.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0431f9.ps} \end{figure}$ Figure 6: The widths (w) as a function of the inner shifts of the broad Gaussian components obtained for the H $\alpha$ and H $\beta$ lines of our sample of AGNs (open circles) and the Fe II template (full triangles).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0431f10.ps}\end{figure}$ Figure 7: The Gaussian width of the Fe II template ( $w_{\rm FeII}$ ) as a function of the central broad Gaussian component width ( $w_{\rm C}$ ) of the H $\alpha$ (open triangles) and H $\beta$ (open circles) line. The solid line corresponds to $w_{\rm FeII}=w_{\rm C}$ and the dashed one to $w_{\rm FeII}=2\cdot w_{\rm C}$ . The points at the top, outside of the region between the two lines belong to 3C 273.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0431f11.ps} \end{figure}$ Figure 8: The comparison of H $\beta$ and H $\alpha$ (dashed lines) profiles with an averaged one (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=4.1cm,clip]{0431f12.ps}\hspace*{3mm} \includegraphics[width=4.1cm,clip]{0431f13.ps} \end{figure}$ Figure 9: Two fits of 3C 273 with the two-component model. The disk parameters are: a) $i=14^\circ$ , $R_{\rm inn}=400$ $R_{\rm g}$ , $R_{\rm out}=1420~R_{\rm g}$ , $W_{\rm d}=1620$ km s^-1, p=3.0 ( $W_{\rm G}=1350$ km s^-1); b) $i=29^\circ$ , $R_{\rm inn}=1250~R_{\rm g}$ , $R_{\rm out}=15~000~R_{\rm g}$ , $W_{\rm d}=700$ km s^-1, p=2.8( $W_{\rm G}=1380$ km s^-1).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0431f14.ps} \end{figure}$ Figure 10: The random velocities of a spherical region (ILR) as a function of the local random disk velocities. The dashed line represents the function $V_{\rm ILR}=V_{\rm Disk}$ km s^-1.
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In the text