Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[width=84mm,clip]{3314f1a}\par\includegraphics[width=84mm,clip]{3314f1b} \end{figure}$ Figure 1: Image of the system obtained with MOS1 during the March 03 ( top) and February 05 ( bottom) exposure with contours and used extraction regions (red) for the two components overlayed. Image creation is identical and the counts per image are very similar, the darkening of the $\alpha$ Cen A component at the upper left is striking.
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In the text

$\begin{figure} \par\includegraphics[width=81mm,clip]{3314f2Montage.eps} \end{figure}$ Figure 2: Light curves of $\alpha$ Cen A/B (red/black) in chronological order as extracted from MOS1 data with 10/3 min binning. The plot sizes are identical for all observations to allow better comparison.
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In the text

$\begin{figure} \par\includegraphics[width=50mm,height=85mm,,angle=-90,clip]{3314f4} \end{figure}$ Figure 4: Spectra of the $\alpha$ Cen system obtained with the PN detector: 03/03 (black/top), 07/04 (red/bottom). Despite the different contributions from each component and absolute luminosities, both spectra are very similar and soften only slightly with decreasing flux.
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In the text

$\begin{figure} \par\includegraphics[width=83mm,clip]{3314f5} \end{figure}$ Figure 5: Light curve of the system in two energy bands with the flare on $\alpha$ Cen B that occurred on January, 29, 2004, PN data with 300 s binning. Overlayed on the hard band is a flare model assuming an exponential decay.
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In the text

$\begin{figure} \par\includegraphics[width=84mm,clip]{3314f6} \end{figure}$ Figure 6: Long term light curve of $\alpha$ Cen A and B for the five XMM-Newton observations. Errors are Poissonian errors on the derived counts only.
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In the text

$\begin{figure} \par\includegraphics[width=84mm,clip]{3314f1a}\par\includegraphics[width=84mm,clip]{3314f1b} \end{figure}$	Figure 1: Image of the system obtained with MOS1 during the March 03 ( top) and February 05 ( bottom) exposure with contours and used extraction regions (red) for the two components overlayed. Image creation is identical and the counts per image are very similar, the darkening of the $\alpha$ Cen A component at the upper left is striking.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=81mm,clip]{3314f2Montage.eps} \end{figure}$	Figure 2: Light curves of $\alpha$ Cen A/B (red/black) in chronological order as extracted from MOS1 data with 10/3 min binning. The plot sizes are identical for all observations to allow better comparison.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=83mm,clip]{3314f3} \end{figure}$	Figure 3: The RGS spectrum of the Feb. 05 exposure, an almost pure spectrum of $\alpha$ Cen B.
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$\begin{figure} \par\includegraphics[width=50mm,height=85mm,,angle=-90,clip]{3314f4} \end{figure}$	Figure 4: Spectra of the $\alpha$ Cen system obtained with the PN detector: 03/03 (black/top), 07/04 (red/bottom). Despite the different contributions from each component and absolute luminosities, both spectra are very similar and soften only slightly with decreasing flux.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=83mm,clip]{3314f5} \end{figure}$	Figure 5: Light curve of the system in two energy bands with the flare on $\alpha$ Cen B that occurred on January, 29, 2004, PN data with 300 s binning. Overlayed on the hard band is a flare model assuming an exponential decay.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=84mm,clip]{3314f6} \end{figure}$	Figure 6: Long term light curve of $\alpha$ Cen A and B for the five XMM-Newton observations. Errors are Poissonian errors on the derived counts only.
Open with DEXTER