All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{0497fig1.eps}\vs... ...*{1.5mm} \includegraphics[angle=-90,width=7.8cm,clip]{0497fig3.eps} \end{figure}$ Figure 1: Combined dereddened spectra of the red and blue wavelength range rebinned to rest wavelengths for comparison. A template galaxy spectrum (NGC 3115 or NGC 4179) was subtracted for ESO 103-G035 and TXS 2226-184. The upper observed spectrum of IC 1481 shows strong Balmer absorption lines and weak Ca II H+K features. Thus, a linear combination of A0V - F8V stars and the template galaxy was subtracted (see middle spectrum). The result is shown in the lower spectrum. (Both upper spectra of IC 1481 are shifted vertically by an arbitrary amount.)
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm]{0497fig4.eps}\vspace*... ...space*{1.5mm} \includegraphics[angle=-90,width=8.2cm]{0497fig6.eps} \end{figure}$ Figure 2: Rotation curves of the three H₂O-megamaser galaxies derived from the average value of the H $\alpha$ and [N II] $\lambda$ 6583 peak wavelengths.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm]{0497fig7.eps}\vspace*{1... ...\vspace*{1.5mm} \includegraphics[angle=-90,width=8cm]{0497fig9.eps} \end{figure}$ Figure 3: H $\beta$ and [O III] $\lambda \lambda$ 4959,5007 fit by three Gaussians ( upper), three Lorentzians ( middle) and three d-Lorentzians ( lower) (ESO 103-G035). The total fit is shown (dashed line). Gaussians yield too narrow wings, Lorentzians too broad ones, whereas d-Lorentzians give the best total fit.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm]{0497fig10.eps}\vspace... ...pace*{1.5mm} \includegraphics[angle=-90,width=7.7cm]{0497fig12.eps} \end{figure}$ Figure 4: The same as in Fig. 3 for the H $\alpha$ and [N II] $\lambda \lambda$ 6548, 6583 blend (IC 1481). Again, d-Lorentzians lead to the best total fit.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm]{0497fig13.eps}\vspace*{1.5mm} \includegraphics[angle=-90,width=8cm]{0497fig14.eps} \end{figure}$ Figure A.1: Upper panel: comparison of Gaussian (solid), Lorentzian (dotted) and d-Lorentz functions (dashed line) (a = 100, b = 5000, c = 20 for Gaussian and Lorentzian, c = 26.1 and d = 1.5 for d-Lorentzian to gain the same effective FWHM). A d-Lorentzian falls in between a Gaussian and a Lorentz function. Lower panel: four d-Lorentzians are shown with different d parameters [d = 0.8 (dashed), d = 1.2 (dotted), d = 1.5 (solid) and d = 2 (dash-dotted)]. With increasing d, the wing profile narrows. Thus, the parameter d can be used to adjust the wings.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm]{0497fig4.eps}\vspace... ...space{1.5mm} \includegraphics[angle=-90,width=8.2cm]{0497fig6.eps} \end{figure}$	Figure 2: Rotation curves of the three H₂O-megamaser galaxies derived from the average value of the H $\alpha$ and [N II] $\lambda$ 6583 peak wavelengths.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm]{0497fig7.eps}\vspace{1... ...\vspace{1.5mm} \includegraphics[angle=-90,width=8cm]{0497fig9.eps} \end{figure}$	Figure 3: H $\beta$ and [O III] $\lambda \lambda$ 4959,5007 fit by three Gaussians ( upper), three Lorentzians ( middle) and three d-Lorentzians ( lower) (ESO 103-G035). The total fit is shown (dashed line). Gaussians yield too narrow wings, Lorentzians too broad ones, whereas d-Lorentzians give the best total fit.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm]{0497fig10.eps}\vspace... ...pace*{1.5mm} \includegraphics[angle=-90,width=7.7cm]{0497fig12.eps} \end{figure}$	Figure 4: The same as in Fig. 3 for the H $\alpha$ and [N II] $\lambda \lambda$ 6548, 6583 blend (IC 1481). Again, d-Lorentzians lead to the best total fit.
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