All Figures

$\begin{figure} \par\mbox{\includegraphics[width=9cm, clip]{8851fig1a_cmyk.eps} \includegraphics[width=9cm, clip]{8851fig1b_cmyk.eps} } \end{figure}$ Figure 1: Three-color images of Westerlund 2 in X-rays ( a), left: full field; b), right: central 8 $^\prime$ in the middle and c), below: core of the cluster). The red, green and blue colors correspond to soft (0.3-1 keV), medium (1.-2. keV) and hard (2.-10. keV) photon energies, respectively. The images were corrected by the exposure maps and adaptively smoothed prior to RGB combination.
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In the text

$\begin{figure} \par\includegraphics[width=9cm, clip]{8851fig1c_cmyk.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[height=18cm, angle=-90]{8851fig2a.ps} \end{figure}$ Figure 2: The core of the Westerlund 2 cluster seen in visible ( a), left) and X-rays ( b), right). X-ray contours superimposed on the visible image ( c), below; the X-ray data were adaptively smoothed).
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In the text

$\begin{figure} \par\includegraphics[height=9cm, angle=-90]{8851fig2b.ps} \end{figure}$ Figure 2: continued.
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In the text

$\begin{figure} \par\includegraphics[height=9cm]{8851fig3.ps} \end{figure}$ Figure 3: Full band background-corrected lightcurves in units of counts per 5 ks bin for the three Chandra observations ( earliest at the top, latest at the bottom). Data from MSP18 are shown in the left panel, those of MSP188 in the middle one and those of WR20b in the right one. Note that the first and last bins, when affected by uncompleteness, were discarded and that the first observation of MSP18 was affected by the spacecraft's dithering (thereby explaining the lower number of recorded counts).
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=8cm]{8851fig4a.ps} \includegraphics[height=8cm]{8851fig4b.ps} } \end{figure}$ Figure 4: Left: X-ray luminosity vs. bolometric luminosity. The solid line corresponds to the canonical relation of Sana et al. (2006); the stars represents the Wolf-Rayet objects, the filled circles the brightest O-type stars (see Table 4) and the open circles the faintest ones (see Table 3). Right: hardness ratios, symbols as in the left panel.
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=8cm]{8851fig5a.ps} \includegraphics[height=8cm]{8851fig5b.ps} } \end{figure}$ Figure 5: Left: visible lightcurve of WR20a ( top figure), X-ray lightcurves for the full energy band with bins of 2 ks ( middle figure) and 5 ks ( bottom figure). Right: lightcurve in the medium (M, top) and hard (H, middle) bands, together with evolution of the hardness ratio HR₂=(H-M)/(H+M) with phase ( bottom), all shown in 5 ks bins. The X-ray data from the second observation are shown in solid black circles and those from the third one in open red triangles; uncomplete bins were discarded. The uncertainty on the phase $\sigma _{\phi }$ is about 0.01, taking into account the uncertainty on the period and the time elapsed since our optical observations ( $\sim$ 700 d, Rauw et al. 2007).
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In the text

$\begin{figure} \par\includegraphics[width=16cm, bb=28 416 590 680, clip]{8851fig6.ps} \end{figure}$ Figure 6: Light curves of the eight sources that display a strong flare during one of the Chandra observations of Westerlund 2. The sources are identified as in Table 5 and the number of the observation where the flare occured is also indicated. For each panel the x-axis shows the time (in ks) elapsed since the beginning of the observation. The lightcurves were binned with a time bin of 5 ks but note that the first and last bins might be affected by incompleteness.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{8851fig7.ps} \end{figure}$ Figure 7: (B-V, V) color-magnitude diagram of the X-ray sources that have an optical counterpart within a correlation radius of less than 1 $^{\prime \prime }$ . The dashed lines correspond to the main-sequence between spectral types O3 and B2 for a distance modulus of 14.52 and reddened with A_V = 4.68 (leftmost curve) or 5.84 (rightmost curve) and assuming R_V = 3.1.
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In the text

$\begin{figure} \par\includegraphics[width=9cm, clip]{8851fig1c_cmyk.eps} \end{figure}$	Figure 1: continued.
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$\begin{figure} \par\includegraphics[height=18cm, angle=-90]{8851fig2a.ps} \end{figure}$	Figure 2: The core of the Westerlund 2 cluster seen in visible ( a), left) and X-rays ( b), right). X-ray contours superimposed on the visible image ( c), below; the X-ray data were adaptively smoothed).
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$\begin{figure} \par\includegraphics[height=9cm, angle=-90]{8851fig2b.ps} \end{figure}$	Figure 2: continued.
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$\begin{figure} \par\mbox{\includegraphics[height=8cm]{8851fig4a.ps} \includegraphics[height=8cm]{8851fig4b.ps} } \end{figure}$	Figure 4: Left: X-ray luminosity vs. bolometric luminosity. The solid line corresponds to the canonical relation of Sana et al. (2006); the stars represents the Wolf-Rayet objects, the filled circles the brightest O-type stars (see Table 4) and the open circles the faintest ones (see Table 3). Right: hardness ratios, symbols as in the left panel.
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$\begin{figure} \par\includegraphics[width=8cm]{8851fig7.ps} \end{figure}$	Figure 7: (B-V, V) color-magnitude diagram of the X-ray sources that have an optical counterpart within a correlation radius of less than 1 $^{\prime \prime }$ . The dashed lines correspond to the main-sequence between spectral types O3 and B2 for a distance modulus of 14.52 and reddened with A_V = 4.68 (leftmost curve) or 5.84 (rightmost curve) and assuming R_V = 3.1.
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