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$\begin{figure} \par\resizebox{14cm}{!}{\includegraphics[clip]{1446fig1.eps}}\end{figure}$ Figure 1: FUV emission lines observed in the HD 163296 FUSE (2002/29/04) and HST/STIS spectra. The arrow points to the C II resonance line at 1036 Å, whereas the line labeled with the $\oplus$ symbol, close to the ${\lambda }$ 1037 O VI line, is an airglow emission line. The narrow H₂ absorption lines and the O I fine structure lines, superimposed on the emission profiles are indicated with tic marks. The dotted lines correspond to the blue wing of each emission line reflected about the zero velocity in the stellar rest frame and overplotted on the red wing to highlight the asymmetry of the profile. Note that the emission peak of the second component of the N V doublet at 1242 Å is apparent at about +850 km s^-1 from the first component.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{1446fig2.eps}}\end{figure}$ Figure 2: The H I Ly $\alpha$ line in the STIS spectrum. The dotted line is the reflected profile which provides an estimate of the interstellar contamination to the emission line.
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In the text

$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip]{1446fig3.eps}}\end{figure}$ Figure 3: Temporal variation of the C III^* emission line profile: the FUSE spectrum rebinned by 8 pixels (2001/04/27, solid line) and the STIS spectrum (2000/07/22, dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{1446fig4.eps}\end{figure}$ Figure 4: LiF2a FUSE spectrum of HD 163296 recorded on 2001/04/27. The main emission features identified as Fe II fluorescent decays following excitation by H I Ly $\alpha$ are labeled at the top.
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In the text

$\begin{figure} \par\resizebox{8.6cm}{!}{\includegraphics[clip]{1446fig5.eps}}\end{figure}$ Figure 5: Observed profile of the Mg II k line (full line) from the IUE archives and a synthetic profile (dashed line) computed with ETLA, using $\dot{M}$ = 7.3 $M_{\odot }$ yr^-1.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{1446fig2.eps}}\end{figure}$	Figure 2: The H I Ly $\alpha$ line in the STIS spectrum. The dotted line is the reflected profile which provides an estimate of the interstellar contamination to the emission line.
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$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip]{1446fig3.eps}}\end{figure}$	Figure 3: Temporal variation of the C III^* emission line profile: the FUSE spectrum rebinned by 8 pixels (2001/04/27, solid line) and the STIS spectrum (2000/07/22, dotted line).
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$\begin{figure} \par\includegraphics[width=12cm,clip]{1446fig4.eps}\end{figure}$	Figure 4: LiF2a FUSE spectrum of HD 163296 recorded on 2001/04/27. The main emission features identified as Fe II fluorescent decays following excitation by H I Ly $\alpha$ are labeled at the top.
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$\begin{figure} \par\resizebox{8.6cm}{!}{\includegraphics[clip]{1446fig5.eps}}\end{figure}$	Figure 5: Observed profile of the Mg II k line (full line) from the IUE archives and a synthetic profile (dashed line) computed with ETLA, using $\dot{M}$ = 7.3 $M_{\odot }$ yr^-1.
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