All Figures

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{1717fig1.ps} \par\end{figure}$ Figure 1: Cumulative fraction for a K-S test of ${L/L_{\rm Eddington}}$ for NLS1 with log $\sigma _{\rm [OIII]}<2.25$ (solid line) and log $\sigma _{\rm [OIII]}>2.25$ (dashed line). The two distributions are clearly different. The NLS1s with high ${L/L_{\rm Eddington}}$ occupy a distinct region on the $M_{\rm BH}$ - $\sigma$ plane.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{1717fig2.ps} \end{figure}$ Figure 2: Same as Fig. 1, but for the soft X-ray spectral index $\alpha$ . Again, the two distributions are found to be statistically different. Objects with high ${L/L_{\rm Eddington}}$ also have steep spectra and are the ones lying below the $M_{\rm BH}$ - $\sigma$ relation of normal galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{1717fig3.ps} \end{figure}$ Figure 3: Same as Fig. 1, but for equivalent width of FeII emission. Large ${L/L_{\rm Eddington}}$ , steep $\alpha$ sources also appear to be strong FeII emitters.
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{1717fig1.ps} \par\end{figure}$	Figure 1: Cumulative fraction for a K-S test of ${L/L_{\rm Eddington}}$ for NLS1 with log $\sigma _{\rm [OIII]}<2.25$ (solid line) and log $\sigma _{\rm [OIII]}>2.25$ (dashed line). The two distributions are clearly different. The NLS1s with high ${L/L_{\rm Eddington}}$ occupy a distinct region on the $M_{\rm BH}$ - $\sigma$ plane.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6cm,clip]{1717fig2.ps} \end{figure}$	Figure 2: Same as Fig. 1, but for the soft X-ray spectral index $\alpha$ . Again, the two distributions are found to be statistically different. Objects with high ${L/L_{\rm Eddington}}$ also have steep spectra and are the ones lying below the $M_{\rm BH}$ - $\sigma$ relation of normal galaxies.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6cm,clip]{1717fig3.ps} \end{figure}$	Figure 3: Same as Fig. 1, but for equivalent width of FeII emission. Large ${L/L_{\rm Eddington}}$ , steep $\alpha$ sources also appear to be strong FeII emitters.
Open with DEXTER