All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{6392fig1.ps} \end{figure}$ Figure 1: Average H $\alpha$ profile (full line), the profile of 7 July 2000 and 19 June 2001 (dashed and dotted lines respectively, see Henrichs et al. 2003). During our observations more emission was present than in 2000.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.8cm,clip]{6392fig2.ps} \end{figure}$ Figure 2: Spectro-astrometric observations of H $\alpha$ ( left) and the He I line at 6678 Å ( right) of the $\beta$ Cep system. Shown are the normalised intensity line profile ( top) and the position of the photocentre of the spatial profile relative to that of the continuum ( bottom). In the plot of the offset of the photocentre the results of all individual spectra are shown (dotted lines) as well as the average (full line). In both the H $\alpha$ and He I plots a shift of the photocentre towards the companion is visible. However, in H $\alpha$ the photocentre is offset from about -400 to +400 km s^-1, while in He I the width of the offset is similar to the width of the line.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.2cm,clip]{6392fig3.ps} \end{figure}$ Figure 3: The results of the separation of the spectra of the primary and secondary components. We show the normalised intensity line profile ( top) and the separated line profiles of the primary ( middle) and the secondary ( bottom). For the splitting of the spectra we have assumed a separation of 0.07 $^{\prime \prime }$ (dashed lines), 0.1 $^{\prime \prime }$ (full line, corresponding to the best estimate of the separation), and 0.15 $^{\prime \prime }$ (dotted line). A double-peaked H $\alpha$ emission line with a width of $\sim$ 400 km s^-1, typical of a classical Be star, is found in the secondary star. The He I line at 6678 Å is only present in the primary star.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{6392fig1.ps} \end{figure}$	Figure 1: Average H $\alpha$ profile (full line), the profile of 7 July 2000 and 19 June 2001 (dashed and dotted lines respectively, see Henrichs et al. 2003). During our observations more emission was present than in 2000.
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