All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1701f1.eps}\end{figure}$ Figure 1: H $\alpha$ image of the central 3 $^{\prime \prime }$ $\times$ 3 $^{\prime \prime }$ of NGC 5252 with superposed the three slit locations. North is up, East is left.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1701f2a.eps}\vspace*{3mm} \includegraphics[width=8.5cm,clip]{1701f2b.eps}\end{figure}$ Figure 2: Emission lines profiles on the nucleus ( bottom panel) and at 0 $.\!\!^{\prime\prime}$ 3 NE of the nucleus ( upper panel) showing the regions were the line profile cannot be fitted with a single Gaussian and a high velocity component was added.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1701f3.ps}\end{figure}$ Figure 3: Velocity, FWHM and flux at along the POS1 slit. Positions along the slit are relative to the continuum peak, positive values are SW. The instrumental line-width of 100 ${\rm km~s}^{-1}$ is drawn as a dotted line in the FWHM panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1701f4.ps}\end{figure}$ Figure 4: Same as Fig. 3 for the NUC slit. The patches of disturbed gas, spatially coincident with the off-nuclear line knots, are marked with asterisks. Here lines are fitted with a double Gaussian to separate the broad perturbed component from the rotating gas.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1701f5.ps}\end{figure}$ Figure 5: Same as Fig. 3 for the POS2 slit.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1701f6.ps}\end{figure}$ Figure 6: Central 8 $\times$ 8 arcsec of the NICMOS F160W image of NGC 5252. The compass indicates the North-East orientation. Note the smooth regular shape of the galaxy and the bright central unresolved source.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1701f7.eps}\end{figure}$ Figure 7: Results of the isophotes analysis of the H band images of NGC 5252. Surface brightness is shown in the top panel (in units of erg s^-1 cm^-2 Å^-1 arcsec^-2), the galaxy's ellipticity and position angle are shown in the middle and bottom panels respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1701f8.eps}\end{figure}$ Figure 8: Brightness profile of NGC 5252. Surface brightness is in units of erg s^-1 cm^-2 Å^-1 arcsec^-2. Fit to the profile obtained from an oblate spheroid stellar density distribution with an added nuclear point source.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{1701f9a.eps}\hspace*{2mm} \includegraphics[width=7.9cm,clip]{1701f9b.ps}\end{figure}$ Figure 9: Best fit to the rotation curves ( left), line surface brightness ( upper right panel) and line width ( lower right panel).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1701f10.eps}\end{figure}$ Figure 10: $\chi ^2$ contours at varying $\Upsilon$ and $M_{{\rm BH}}$ for an inclination of 70 $^\circ$ . Contours are plotted for confidence levels of 1, 2 and 3 $\sigma$ . Plotted in a dotted contour is the 1 $\sigma$ confidence level for 45 $^\circ$ , while the plus sign mark the overall best fit.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{1701f11a.ps}\vspace*{5mm} ... ...1b.eps}\vspace*{5mm} \includegraphics[width=5.8cm,clip]{1701f11c.ps}\end{figure}$ Figure 11: ( Top) $M_{{\rm BH}}$ vs. stellar velocity dispersion $\sigma _{\rm c}$ and ( middle) $M_{{\rm BH}}$ vs. bulge mass with the best fits obtained from a bisector linear regression analysis (solid line) and ordinary least-square (dashed line; bottom) residual of the $M_{{\rm BH}}$ - $\sigma _{\rm c}$ correlation vs. $R_{\rm e}$ from Marconi & Hunt (2003).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1701f12a.eps}\hspace*{6mm} \includegraphics[width=7.7cm,clip]{1701f12b.ps}\end{figure}$ Figure 12: Best fit of the rotation curves ( left), to the line surface brightness ( upper right panel) and line width ( lower right panel) obtained for a black mass of $M = 10^8~M_{\odot}$ predicted from the correlation between BHM and velocity dispersion. The dotted lines correspond to the case of no central black hole.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1701f13.ps}\end{figure}$ Figure 13: Residuals between the kinematical models and the observed velocity points on the nuclear slit for the best fit, corresponding to $M_{{\rm BH}}=9.5$ $\times$ $10^8~M_{\odot}$ ( upper panel), for a black hole mass of $M_{{\rm BH}}= 10^8~M_{\odot}$ discussed in Sect. 5 ( middle panel) and for the case without central black hole ( lower panel).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1701f14.eps}\end{figure}$ Figure 14: Host galaxy's magnitude versus black hole mass for radio-quiet QSO (open circles), radio-loud QSO (filled circles) and Seyfert 1 (squares) taken from McLure & Dunlop (2001). The cross marks the location of NGC 5252 in this plane that falls in the region populated by QSO.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1701f1.eps}\end{figure}$	Figure 1: H $\alpha$ image of the central 3 $^{\prime \prime }$ $\times$ 3 $^{\prime \prime }$ of NGC 5252 with superposed the three slit locations. North is up, East is left.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1701f2a.eps}\vspace*{3mm} \includegraphics[width=8.5cm,clip]{1701f2b.eps}\end{figure}$	Figure 2: Emission lines profiles on the nucleus ( bottom panel) and at 0 $.\!\!^{\prime\prime}$ 3 NE of the nucleus ( upper panel) showing the regions were the line profile cannot be fitted with a single Gaussian and a high velocity component was added.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1701f3.ps}\end{figure}$	Figure 3: Velocity, FWHM and flux at along the POS1 slit. Positions along the slit are relative to the continuum peak, positive values are SW. The instrumental line-width of 100 ${\rm km~s}^{-1}$ is drawn as a dotted line in the FWHM panel.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1701f4.ps}\end{figure}$	Figure 4: Same as Fig. 3 for the NUC slit. The patches of disturbed gas, spatially coincident with the off-nuclear line knots, are marked with asterisks. Here lines are fitted with a double Gaussian to separate the broad perturbed component from the rotating gas.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1701f5.ps}\end{figure}$	Figure 5: Same as Fig. 3 for the POS2 slit.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1701f6.ps}\end{figure}$	Figure 6: Central 8 $\times$ 8 arcsec of the NICMOS F160W image of NGC 5252. The compass indicates the North-East orientation. Note the smooth regular shape of the galaxy and the bright central unresolved source.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1701f7.eps}\end{figure}$	Figure 7: Results of the isophotes analysis of the H band images of NGC 5252. Surface brightness is shown in the top panel (in units of erg s^-1 cm^-2 Å^-1 arcsec^-2), the galaxy's ellipticity and position angle are shown in the middle and bottom panels respectively.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1701f8.eps}\end{figure}$	Figure 8: Brightness profile of NGC 5252. Surface brightness is in units of erg s^-1 cm^-2 Å^-1 arcsec^-2. Fit to the profile obtained from an oblate spheroid stellar density distribution with an added nuclear point source.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{1701f9a.eps}\hspace*{2mm} \includegraphics[width=7.9cm,clip]{1701f9b.ps}\end{figure}$	Figure 9: Best fit to the rotation curves ( left), line surface brightness ( upper right panel) and line width ( lower right panel).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1701f10.eps}\end{figure}$	Figure 10: $\chi ^2$ contours at varying $\Upsilon$ and $M_{{\rm BH}}$ for an inclination of 70 $^\circ$ . Contours are plotted for confidence levels of 1, 2 and 3 $\sigma$ . Plotted in a dotted contour is the 1 $\sigma$ confidence level for 45 $^\circ$ , while the plus sign mark the overall best fit.
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{1701f11a.ps}\vspace{5mm} ... ...1b.eps}\vspace{5mm} \includegraphics[width=5.8cm,clip]{1701f11c.ps}\end{figure}$	Figure 11: ( Top) $M_{{\rm BH}}$ vs. stellar velocity dispersion $\sigma _{\rm c}$ and ( middle) $M_{{\rm BH}}$ vs. bulge mass with the best fits obtained from a bisector linear regression analysis (solid line) and ordinary least-square (dashed line; bottom) residual of the $M_{{\rm BH}}$ - $\sigma _{\rm c}$ correlation vs. $R_{\rm e}$ from Marconi & Hunt (2003).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1701f12a.eps}\hspace*{6mm} \includegraphics[width=7.7cm,clip]{1701f12b.ps}\end{figure}$	Figure 12: Best fit of the rotation curves ( left), to the line surface brightness ( upper right panel) and line width ( lower right panel) obtained for a black mass of $M = 10^8~M_{\odot}$ predicted from the correlation between BHM and velocity dispersion. The dotted lines correspond to the case of no central black hole.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1701f13.ps}\end{figure}$	Figure 13: Residuals between the kinematical models and the observed velocity points on the nuclear slit for the best fit, corresponding to $M_{{\rm BH}}=9.5$ $\times$ $10^8~M_{\odot}$ ( upper panel), for a black hole mass of $M_{{\rm BH}}= 10^8~M_{\odot}$ discussed in Sect. 5 ( middle panel) and for the case without central black hole ( lower panel).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1701f14.eps}\end{figure}$	Figure 14: Host galaxy's magnitude versus black hole mass for radio-quiet QSO (open circles), radio-loud QSO (filled circles) and Seyfert 1 (squares) taken from McLure & Dunlop (2001). The cross marks the location of NGC 5252 in this plane that falls in the region populated by QSO.
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