All Figures

$\begin{figure} \par\includegraphics[width=8.9cm,height=8.5cm]{H4193F1.ps} \end{figure}$ Figure 1: Observed (thick line) and computed (thin line, R = 100) flux distribution of HD 207538. The ATLAS9 atmosphere model has been computed assuming $T_{\rm eff}=32190$ K, $\log g=4.32$ , solar metal opacity and microturbulence velocity equal to 8.0 km s^-1. Because of the presence of large absorption due to the interstellar medium, FUSE data are averaged within 2 Å-width bands centered at the highest values of the flux distribution in order to visualize the differences between the observed and computed spectra (filled squares). The extinction bump at $\lambda$ 2175 Å is clearly visible on this plot.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16.4cm,clip]{H4193F2.ps} \end{figure}$ Figure 2: Comparison between theoretical (smoothed line) and observed spectra in the visible range $\lambda \lambda$ 4625-4720 Å (top panel) and $\lambda \lambda 5650$ -5750 (bottom panel). In each panel we label the identified lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{H4193F3.ps} \end{figure}$ Figure 3: Helium lines observed (dotted line) in the visible spectrum of HD 207538. For each line we overplotted the corresponding synthetic profile (solid/red curve).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{H4193F4.ps} \end{figure}$ Figure 4: Comparison between theoretical and observed spectra in the IUE range selected ( $\lambda \lambda$ 1380-1670) Å. In each panel we label the identified lines. ISM lines have been marked with arrows.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{H4193F5.ps} \end{figure}$ Figure 5: Fits of the Na I absorption lines. Three components are detected, the central components represents more that 99% of the total column density: $5.3 \times 10^{14}$ cm^-2.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{H4193F6.ps} \end{figure}$ Figure 6: Comparison of elemental abundances with respect to hydrogen in the standard logarithmic scale (Grevesse & Sauval 1998). Open diamonds represent the measurements toward HD207538 and black diamonds represent the solar references.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{H4193F7.ps}\end{figure}$ Figure 7: Comparison between theoretical and observed spectra in the FUV range $\lambda$ 1000-1098 Å. In each box we have: at the top the ISM model with labelled the identified lines, at the middle the synthetic photospheric model with the identified lines and at the bottom, the observed spectrum compared with the total model.
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In the text

$\begin{figure} \par\includegraphics[width=17.1cm,clip]{H4193F8.ps} \end{figure}$ Figure 8: Comparison between theoretical and observed spectra in the FUV range $\lambda$ 1098-1188 Å. Symbols as in Fig. 7.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16.4cm,clip]{H4193F2.ps} \end{figure}$	Figure 2: Comparison between theoretical (smoothed line) and observed spectra in the visible range $\lambda \lambda$ 4625-4720 Å (top panel) and $\lambda \lambda 5650$ -5750 (bottom panel). In each panel we label the identified lines.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{H4193F3.ps} \end{figure}$	Figure 3: Helium lines observed (dotted line) in the visible spectrum of HD 207538. For each line we overplotted the corresponding synthetic profile (solid/red curve).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{H4193F4.ps} \end{figure}$	Figure 4: Comparison between theoretical and observed spectra in the IUE range selected ( $\lambda \lambda$ 1380-1670) Å. In each panel we label the identified lines. ISM lines have been marked with arrows.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{H4193F5.ps} \end{figure}$	Figure 5: Fits of the Na I absorption lines. Three components are detected, the central components represents more that 99% of the total column density: $5.3 \times 10^{14}$ cm^-2.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{H4193F6.ps} \end{figure}$	Figure 6: Comparison of elemental abundances with respect to hydrogen in the standard logarithmic scale (Grevesse & Sauval 1998). Open diamonds represent the measurements toward HD207538 and black diamonds represent the solar references.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{H4193F7.ps}\end{figure}$	Figure 7: Comparison between theoretical and observed spectra in the FUV range $\lambda$ 1000-1098 Å. In each box we have: at the top the ISM model with labelled the identified lines, at the middle the synthetic photospheric model with the identified lines and at the bottom, the observed spectrum compared with the total model.
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$\begin{figure} \par\includegraphics[width=17.1cm,clip]{H4193F8.ps} \end{figure}$	Figure 8: Comparison between theoretical and observed spectra in the FUV range $\lambda$ 1098-1188 Å. Symbols as in Fig. 7.
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