Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=16cm,clip]{0190fig1.eps}\end{figure}$ Figure 1: Mean spectra of AC211 in and out of eclipse (orbital-motion-corrected averages of 3 and 12 spectra respectively), obtained with the HST/STIS (see Sect. 2 for details). The mean eclipse spectrum, in which the continuum flux is $0.71 \times 10^{-15} \ {\rm erg~cm}^{-2}~{\rm s}^{-1}~{\rm \AA}^{-1}$ , has been offset for clarity. The error bars for both spectra are smaller than the line thickness. The bottom panel is the eclipse spectrum divided by the out-of-eclipse spectrum, which reveals no evidence of the companion star.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0190fig2.eps}\end{figure}$ Figure 2: Continuum flux through eclipse, measured from our HST/STIS spectra.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{0190fig3.eps}\end{figure}$ Figure 3: Radial velocities of the He I $\lambda {6678}$ P Cyg components.
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In the text

$\begin{figure} \par\includegraphics[width=8.01cm,clip]{0190fig4.eps}\end{figure}$ Figure 4: The He I $\lambda {6678}$ line profiles (the solid lines superimposed on each spectrum are the best-fitting profiles modelled by pairs of Gaussians) with simple representations of an LMXB plotted alongside for each orbital phase. Two sets of cartoons are calculated, using mass ratios M₂/ $M_{\rm x}$ of 0.57 ( left) and 0.10 ( right). The binary inclination assumed is 84 $^{\circ }$ . The cartoons are simple and do not adequately represent the stream/disc impact region and disc bulge, which in reality expends along the disc rim for almost 90 $^{\circ }$ ahead of the stream/disc impact site.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0190fig2.eps}\end{figure}$	Figure 2: Continuum flux through eclipse, measured from our HST/STIS spectra.
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$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{0190fig3.eps}\end{figure}$	Figure 3: Radial velocities of the He I $\lambda {6678}$ P Cyg components.
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