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$\begin{figure} \par\resizebox{8.2cm}{!}{\includegraphics[angle=-90,clip]{f_final2.ps}} \end{figure}$ Figure 1: Example of the rest frame emission-line spectrum obtained for one of the objects in our sample after correction of the stellar contribution; the remaining 18 emission-line spectra are available in electronic form at http://www.edpsciences.org.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[clip]{fits1-2b.eps}} \end{figure}$ Figure 2: Best fitting results for six nuclear emission-line regions; for each object, the blue spectral region is shown on the left panel and the red spectral region on the right panel. The data points are represented by crosses; the solid line is the best fit; the dotted lines show the individual components; the lower crosses give the residuals. Both the data and the models were shifted upwards by an arbitrary amount for the sake of clarity. The residuals give an appreciation of the fit quality; in this figure, they are of the same order of magnitude as the noise in the spectra.
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In the text

$\begin{figure} \par\resizebox{11.8cm}{!}{\includegraphics[clip]{dd.eps}}\hfill \parbox[b]{55mm}{ } \end{figure}$ Figure 3: Diagnostic diagrams showing the logarithm of O III $\lambda$ 5007/H $\beta$ vs. N II $\lambda$ 6584/H $\alpha$ and O III $\lambda$ 5007/H $\beta$ vs. O I $\lambda$ 6300/H $\alpha$ . Most of the objects in our sample are located in the LINER region (represented as dots). Only a few nuclei display a higher excitation spectrum, occupying the same location as Seyfert galaxies (represented as triangles). The estimated errors are of the order of 0.10 and 0.13 in the x-axis (logN II $\lambda$ 6584/H $\alpha$ and logO I $\lambda$ 65300/H $\alpha$ , respectively) and 0.11 in the y-axis.
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In the text

Full Version

$\begin{figure} \par\resizebox{8.2cm}{!}{\includegraphics[angle=-0,clip]{fig4_nova_crop.ps}} \end{figure}$ Figure 1: The rest frame emission-line spectrum obtained for one of the objects in our sample after correction of the stellar contribution.
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In the text

$\begin{figure} \par\resizebox{8.2cm}{!}{\includegraphics[angle=-0,clip]{fig5_nova_crop.ps}} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\resizebox{8.2cm}{!}{\includegraphics[angle=-0,clip]{fig6_nova_crop.ps}} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\resizebox{8.2cm}{!}{\includegraphics[angle=-90,clip]{f_final2.ps}} \end{figure}$	Figure 1: Example of the rest frame emission-line spectrum obtained for one of the objects in our sample after correction of the stellar contribution; the remaining 18 emission-line spectra are available in electronic form at http://www.edpsciences.org.
Open with DEXTER

$\begin{figure} \par\resizebox{8.2cm}{!}{\includegraphics[angle=-0,clip]{fig4_nova_crop.ps}} \end{figure}$	Figure 1: The rest frame emission-line spectrum obtained for one of the objects in our sample after correction of the stellar contribution.
Open with DEXTER

$\begin{figure} \par\resizebox{8.2cm}{!}{\includegraphics[angle=-0,clip]{fig5_nova_crop.ps}} \end{figure}$	Figure 1: continued.
Open with DEXTER