Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[height=6.2cm,width=7.7cm,clip]{35fig1.ps} \end{figure}$ Figure 1: Sketch of the $\gamma ^2$ Vel orbital configuration at the phases of our X-ray observations. The Wolf-Rayet star is at the center. Shape and orientation of the wind blown cavities around the O star are schematic only.
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In the text

$\begin{figure} \par\includegraphics[height=6cm,width=8.8cm,clip]{35fig2.eps} \end{figure}$ Figure 2: First order background subtracted XMM- RGS spectra of $\gamma ^2$ Vel, corrected for effective area. The spectra observed at high ( $\phi$ = 0.11) and low state ( $\phi$ = 0.37) are plotted. The inset shows a blow-up of the $\phi$ = 0.37 observation.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{35fig3.ps} \end{figure}$ Figure 3: Observed C VI recombination continuum with the theoretically calculated energy distribution folded with the XMM- RGS response function. The profiles correspond to electron temperatures $T_{\rm e}$ = 80 000 K, 40 000 K, and 20 000 K (from wide to narrow).
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In the text

$\begin{figure} \par\includegraphics[width=6.1cm,height=8.6cm,angle=-90,clip]{35f... ...cludegraphics[width=6.1cm,height=8.6cm,angle=-90,clip]{35fig4bo.ps} \end{figure}$ Figure 4: Ne IX triplet consisting of a resonance line (r), an intercombination line (i), and a forbidden line (f) for $\gamma ^2$ Vel ( top and center) and for the O9.7Ib star $\zeta$ Ori ( bottom), observed with XMM- RGS. Note the difference in the forbidden line.
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In the text

$\begin{figure} \par\includegraphics[height=6.8cm,width=8.8cm,clip]{35fig5.ps} \end{figure}$ Figure 5: XMM- EPIC-MOS data of $\gamma ^2$ Vel at low and high state (full lines), observed in 2001. The dotted line is the high state spectrum absorbed by the column density predicted by a smooth WR wind model. The dashed line is the same with a column density reduced by a factor of 4 (see text).
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In the text

$\begin{figure} \par\includegraphics[width=5.3cm,height=8.5cm,angle=-90,clip]{35f... ...cludegraphics[width=5.3cm,height=8.5cm,angle=-90,clip]{35fig6bo.ps} \end{figure}$ Figure 6: The data points show the first-order background-subtracted XMM- EPIC-MOS and - RGS spectra at phases $\phi$ = 0.11 (high state; upper panel) and $\phi$ = 0.37 (low state; lower panel). Error bars correspond to 1 $\sigma$ statistical errors including the effect of background. The plotted curves show our best-fit model.
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In the text

$\begin{figure} \par\includegraphics[width=4.6cm,height=8.5cm,angle=-90,clip]{fig... ...cludegraphics[width=4.6cm,height=8.5cm,angle=-90,clip]{fig7rig4.ps} \end{figure}$ Figure 7: Background-subtracted XMM- EPIC-MOS spectra of $\gamma ^2$ Vel at phases $\phi$ = 0.11 (high state; left panels) and $\phi$ = 0.37 (low state; right panels). Error bars correspond to 1 $\sigma$ statistical errors including the effect of background. The curves show from top to bottom our best-fit total model, and the components 1, 2, and 3, respectively. Some prominent lines are labeled with the emitting ions.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=5.4cm,angle=-90,clip]{35fig... ...includegraphics[height=8cm,width=5.4cm,angle=-90,clip]{35fig8bo.ps} \end{figure}$ Figure 8: DEM modeling of the XMM- EPIC-MOS and - RGS spectra of $\gamma ^2$ Vel ( top: high state; bottom: low state). The emission measure EM per logarithmic temperature bin is in units of 10⁵⁸ cm^-3.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,height=7.7cm,clip]{35fig9.ps} \end{figure}$ Figure 9: Sketch of the $\gamma ^2$ Vel system (same as Fig. 1) with the probable locations of our components 1 to 4. The Wolf-Rayet star is at the center.
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In the text

$\begin{figure} \par\includegraphics[height=6.2cm,width=7.7cm,clip]{35fig1.ps} \end{figure}$	Figure 1: Sketch of the $\gamma ^2$ Vel orbital configuration at the phases of our X-ray observations. The Wolf-Rayet star is at the center. Shape and orientation of the wind blown cavities around the O star are schematic only.
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$\begin{figure} \par\includegraphics[height=6cm,width=8.8cm,clip]{35fig2.eps} \end{figure}$	Figure 2: First order background subtracted XMM- RGS spectra of $\gamma ^2$ Vel, corrected for effective area. The spectra observed at high ( $\phi$ = 0.11) and low state ( $\phi$ = 0.37) are plotted. The inset shows a blow-up of the $\phi$ = 0.37 observation.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{35fig3.ps} \end{figure}$	Figure 3: Observed C VI recombination continuum with the theoretically calculated energy distribution folded with the XMM- RGS response function. The profiles correspond to electron temperatures $T_{\rm e}$ = 80 000 K, 40 000 K, and 20 000 K (from wide to narrow).
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$\begin{figure} \par\includegraphics[width=6.1cm,height=8.6cm,angle=-90,clip]{35f... ...cludegraphics[width=6.1cm,height=8.6cm,angle=-90,clip]{35fig4bo.ps} \end{figure}$	Figure 4: Ne IX triplet consisting of a resonance line (r), an intercombination line (i), and a forbidden line (f) for $\gamma ^2$ Vel ( top and center) and for the O9.7Ib star $\zeta$ Ori ( bottom), observed with XMM- RGS. Note the difference in the forbidden line.
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$\begin{figure} \par\includegraphics[height=6.8cm,width=8.8cm,clip]{35fig5.ps} \end{figure}$	Figure 5: XMM- EPIC-MOS data of $\gamma ^2$ Vel at low and high state (full lines), observed in 2001. The dotted line is the high state spectrum absorbed by the column density predicted by a smooth WR wind model. The dashed line is the same with a column density reduced by a factor of 4 (see text).
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$\begin{figure} \par\includegraphics[width=5.3cm,height=8.5cm,angle=-90,clip]{35f... ...cludegraphics[width=5.3cm,height=8.5cm,angle=-90,clip]{35fig6bo.ps} \end{figure}$	Figure 6: The data points show the first-order background-subtracted XMM- EPIC-MOS and - RGS spectra at phases $\phi$ = 0.11 (high state; upper panel) and $\phi$ = 0.37 (low state; lower panel). Error bars correspond to 1 $\sigma$ statistical errors including the effect of background. The plotted curves show our best-fit model.
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$\begin{figure} \par\includegraphics[height=8cm,width=5.4cm,angle=-90,clip]{35fig... ...includegraphics[height=8cm,width=5.4cm,angle=-90,clip]{35fig8bo.ps} \end{figure}$	Figure 8: DEM modeling of the XMM- EPIC-MOS and - RGS spectra of $\gamma ^2$ Vel ( top: high state; bottom: low state). The emission measure EM per logarithmic temperature bin is in units of 10⁵⁸ cm^-3.
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$\begin{figure} \par\includegraphics[width=8.4cm,height=7.7cm,clip]{35fig9.ps} \end{figure}$	Figure 9: Sketch of the $\gamma ^2$ Vel system (same as Fig. 1) with the probable locations of our components 1 to 4. The Wolf-Rayet star is at the center.
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