All Figures

$\begin{figure} \par\includegraphics[width=14.7cm,clip]{8313fig1.ps} \end{figure}$ Figure 1: The mean deredshifted HET spectrum of Mark 110. The upper panel shows the spectrum. In the lower panel it is scaled to show the weak emission features. The residuals of the best fit are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{8313fig2.ps} \end{figure}$ Figure 2: The upper panel shows the H $\beta$ flux of the very broad system (B1) vs. the continuum flux, while the lower panel shows the He II $\lambda$ 4686 flux of this same system vs. the continuum flux. In the lower panel, the curve shows the continuum at the power 2.3. The continuum fluxes are in units of 10^-15 erg s^-1 cm^-2 Å^-1, while the line intensities are in units of 10^-15 erg s^-1 cm^-2.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8313fig3.ps} \end{figure}$ Figure 3: The upper panel shows the difference between two spectra of Mark 110 having the same continuum level. The very broad line system (B1) has completely disappeared. The only lines visible belong to the narrower broad line system (B3). The lower panel shows the difference between the mean spectrum of the four strongest spectra and the mean spectrum of the four weakest spectra.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{8313fig4.ps} \end{figure}$ Figure 4: a) Fit of the mean of the four strongest spectra of Mark 110 in the region around He II $\lambda$ 4686 and He I $\lambda$ 4713. The dotted line shows the observations; the continuous line is the best fit. The lowest line represents the residuals. We also show the three He I and He II variable components. The locations of the strongest narrow lines are indicated. b) The same for the mean of the four weakest spectra.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{8313fig5.ps} \end{figure}$ Figure 5: Spectra of three NLS1s. Fluxes are in units of 10^-15 erg s^-1 cm^-2 Å^-1. As shown in the text, although Mark 110 has narrow "broad'' emission lines, it is probably not a genuine NLS1.
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In the text

$\begin{figure} \par\includegraphics[width=14.7cm,clip]{8313fig1.ps} \end{figure}$	Figure 1: The mean deredshifted HET spectrum of Mark 110. The upper panel shows the spectrum. In the lower panel it is scaled to show the weak emission features. The residuals of the best fit are also shown.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{8313fig3.ps} \end{figure}$	Figure 3: The upper panel shows the difference between two spectra of Mark 110 having the same continuum level. The very broad line system (B1) has completely disappeared. The only lines visible belong to the narrower broad line system (B3). The lower panel shows the difference between the mean spectrum of the four strongest spectra and the mean spectrum of the four weakest spectra.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{8313fig5.ps} \end{figure}$	Figure 5: Spectra of three NLS1s. Fluxes are in units of 10^-15 erg s^-1 cm^-2 Å^-1. As shown in the text, although Mark 110 has narrow "broad'' emission lines, it is probably not a genuine NLS1.
Open with DEXTER