All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig1.ps} \end{figure}$ Figure 1: Nuclear spectra of NGC 5077: at the slit center position ( upper panels), showing the possible presence of a weak broad H $\alpha$ component, and at 0 $.\!\!^{\prime\prime}$ 1 from it ( lower panels). The best model spectrum (dashed line) is superposed on the data; dotted lines are for the Gaussians and linear continuum components of the fit. Flux is in units of 10^-15 erg cm^-2 s^-1 Å^-1 arcsec^-2. The residuals from the fits are shown in the smaller panels.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig2.ps} \end{figure}$ Figure 2: Upper panel: velocity curve from the off-nuclear slit with the best quality of data. Lower panels: velocity, surface brightness, and velocity dispersion along NUC slit. Surface brightness is in units of 10^-15 erg s^-1 cm^-2 arcsec^-2. Positions along the slit are relative to the continuum peak.
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In the text

$\begin{figure} \par\includegraphics[width=5.3cm,clip]{8570fig3a.ps}\hspace*{4mm}... ....ps}\hspace*{4mm} \includegraphics[width=4.9cm,clip]{8570fig3c.ps} \end{figure}$ Figure 3: Velocity, surface brightness, and velocity dispersion along the off-nuclear slit position N1 ( left panel), NUC ( central panel), and S1 ( right). Positions along the slits are relative to the continuum peak, positive values are NW.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig4.ps} \end{figure}$ Figure 4: Same as Fig. 2. Second upper panel: over-plot of NUC ( empty squares) and S1 ( filled circles) velocity curves showing the inconsistency of the gas position-velocity diagram with regular rotation of a nuclear gas disk.
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In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{8570fig5.ps} \end{figure}$ Figure 5: Left: V band ( F547M filter) image of NGC 5077. Right: H $\alpha$ WFPC2/HST image. Field of view $4\hbox{$.\!\!^{\prime\prime}$ }5 \times 4\hbox{$.\!\!^{\prime\prime}$ }5$ . North is up, East is left.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{8570fig6.ps} \end{figure}$ Figure 6: Results of the isophotes analysis of the V band image of NGC 5077. Surface brightness is shown in the top panel (in units of erg s^-1 cm^-2 Å^-1 arcsec^-2), and the galaxy's ellipticity and position angle are shown in the middle and bottom panels, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{8570fig7.ps} \end{figure}$ Figure 7: Fit to the surface brightness profile obtained from an oblate spheroid stellar density distribution.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig8a.ps}\hspace*{4mm} \includegraphics[width=8cm,clip]{8570fig8b.ps} \end{figure}$ Figure 8: Overall best fit to the rotation curves ( left) with the case of null BH mass (dashed line) superposed on the central slit. Corresponding fit to the line surface brightness distribution ( right). From upper to bottom panel: N1, NUC, S1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig9.ps} \end{figure}$ Figure 9: Upper panel: best fit values of $M_{\rm BH}$ obtained by varying the disk inclination. The continuous line reproduces the $\propto$ 1/ $\sin ^2 i$ dependence of $M_{\rm BH}$ . Lower panel: corresponding $\chi ^2_{r}$ values scaled to the overall best fit. Inclinations smaller than 35 $^\circ$ or larger than 50 $^\circ$ are excluded at a confidence level of 1 $\sigma$ (shaded regions in the diagrams), evaluated for 16 degrees of freedom.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig10.ps} \end{figure}$ Figure 10: $\chi ^2_{r}$ contours at varying ${\it\Upsilon _V}$ and $M_{\rm BH}$ at an inclination of $i = 40^\circ$ . Contours are plotted for confidence levels of 1, 2, and 3 $\sigma$ . The plus sign marks the overall best fit.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig11.ps} \end{figure}$ Figure 11: Velocity dispersion distribution expected from the overall best fit model (solid line) at $i = 40^\circ$ , and derived (dashed line) by including the observed velocity dispersions in the fitting procedure. From upper to bottom panel: N1, NUC, S1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig12.ps} \end{figure}$ Figure 12: $M_{\rm BH}$ vs. bulge mass from Marconi & Hunt (2003) with the best fit obtained from a bisector linear regression analysis (solid line). The positions of NGC 5077 and NGC 3998 are shown by empty circles.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig13a.ps}\par\vspace*{2mm} \includegraphics[width=8cm,clip]{8570fig13b.ps} \end{figure}$ Figure 13: $M_{\rm BH}$ vs. central stellar velocity dispersion from Tremaine et al. (2002) ( upper panel) and from Ferrarese & Ford (2005) ( lower panel). Solid lines indicate the best fits for the two correlations. The positions of NGC 5077 and NGC 3998 are shown by empty circles.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig14.ps} \end{figure}$ Figure 14: Residuals from the $M_{\rm BH}$ vs. $\sigma$ correlation (in the Tremaine et al. form) reported against the bulge effective radius $R_{\rm e}$ . The positions of NGC 5077 and NGC 3998 are indicated by empty circles.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig2.ps} \end{figure}$	Figure 2: Upper panel: velocity curve from the off-nuclear slit with the best quality of data. Lower panels: velocity, surface brightness, and velocity dispersion along NUC slit. Surface brightness is in units of 10^-15 erg s^-1 cm^-2 arcsec^-2. Positions along the slit are relative to the continuum peak.
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$\begin{figure} \par\includegraphics[width=5.3cm,clip]{8570fig3a.ps}\hspace{4mm}... ....ps}\hspace{4mm} \includegraphics[width=4.9cm,clip]{8570fig3c.ps} \end{figure}$	Figure 3: Velocity, surface brightness, and velocity dispersion along the off-nuclear slit position N1 ( left panel), NUC ( central panel), and S1 ( right). Positions along the slits are relative to the continuum peak, positive values are NW.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig4.ps} \end{figure}$	Figure 4: Same as Fig. 2. Second upper panel: over-plot of NUC ( empty squares) and S1 ( filled circles) velocity curves showing the inconsistency of the gas position-velocity diagram with regular rotation of a nuclear gas disk.
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$\begin{figure} \par\includegraphics[width=11.5cm,clip]{8570fig5.ps} \end{figure}$	Figure 5: Left: V band ( F547M filter) image of NGC 5077. Right: H $\alpha$ WFPC2/HST image. Field of view $4\hbox{$.\!\!^{\prime\prime}$ }5 \times 4\hbox{$.\!\!^{\prime\prime}$ }5$ . North is up, East is left.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{8570fig6.ps} \end{figure}$	Figure 6: Results of the isophotes analysis of the V band image of NGC 5077. Surface brightness is shown in the top panel (in units of erg s^-1 cm^-2 Å^-1 arcsec^-2), and the galaxy's ellipticity and position angle are shown in the middle and bottom panels, respectively.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{8570fig7.ps} \end{figure}$	Figure 7: Fit to the surface brightness profile obtained from an oblate spheroid stellar density distribution.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig8a.ps}\hspace*{4mm} \includegraphics[width=8cm,clip]{8570fig8b.ps} \end{figure}$	Figure 8: Overall best fit to the rotation curves ( left) with the case of null BH mass (dashed line) superposed on the central slit. Corresponding fit to the line surface brightness distribution ( right). From upper to bottom panel: N1, NUC, S1.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig10.ps} \end{figure}$	Figure 10: $\chi ^2_{r}$ contours at varying ${\it\Upsilon _V}$ and $M_{\rm BH}$ at an inclination of $i = 40^\circ$ . Contours are plotted for confidence levels of 1, 2, and 3 $\sigma$ . The plus sign marks the overall best fit.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig11.ps} \end{figure}$	Figure 11: Velocity dispersion distribution expected from the overall best fit model (solid line) at $i = 40^\circ$ , and derived (dashed line) by including the observed velocity dispersions in the fitting procedure. From upper to bottom panel: N1, NUC, S1.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig12.ps} \end{figure}$	Figure 12: $M_{\rm BH}$ vs. bulge mass from Marconi & Hunt (2003) with the best fit obtained from a bisector linear regression analysis (solid line). The positions of NGC 5077 and NGC 3998 are shown by empty circles.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig13a.ps}\par\vspace*{2mm} \includegraphics[width=8cm,clip]{8570fig13b.ps} \end{figure}$	Figure 13: $M_{\rm BH}$ vs. central stellar velocity dispersion from Tremaine et al. (2002) ( upper panel) and from Ferrarese & Ford (2005) ( lower panel). Solid lines indicate the best fits for the two correlations. The positions of NGC 5077 and NGC 3998 are shown by empty circles.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8570fig14.ps} \end{figure}$	Figure 14: Residuals from the $M_{\rm BH}$ vs. $\sigma$ correlation (in the Tremaine et al. form) reported against the bulge effective radius $R_{\rm e}$ . The positions of NGC 5077 and NGC 3998 are indicated by empty circles.
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