Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5422fig1.ps} \end{figure}$ Figure 1: Light curves of AB Aur, combining counts from both MOS detectors, binned to 5 ks. Panels from top to bottom: Soft counts in the 0.3-1 keV range; hard counts in the 1-4 keV range; counts in the combined range, 0.3-4 keV; hardness, defined by the ratio of hard to soft counts.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{5422fig3.ps} \end{figure}$ Figure 3: Fluxed, coadded RGS1+RGS2 spectra of SU Aur ( top) and AB Aur ( bottom). The spectra are background subtracted.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{5422fig4.ps} \end{figure}$ Figure 4: Data and fitted spectrum of AB Aur (EMD model). The best-fit model is shown by the histograms in the wavelength region used for the fit. For plotting purposes, the MOS2 spectrum has been shifted along the y-axis by 0.001 cts s^-1 Å^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=7.8cm,clip]{5422fig6.ps} \end{figure}$ Figure 6: Fit of the O VII triplet using variable electron density. The solid histogram gives the best fit ( $n_{\rm e} < 10^{10}$ cm^-3), while the dotted histogram is for the 90% upper limit to $n_{\rm e}$ ( $n_{\rm e} < 1.3\times 10^{11}$ cm^-3).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5422fig1.ps} \end{figure}$	Figure 1: Light curves of AB Aur, combining counts from both MOS detectors, binned to 5 ks. Panels from top to bottom: Soft counts in the 0.3-1 keV range; hard counts in the 1-4 keV range; counts in the combined range, 0.3-4 keV; hardness, defined by the ratio of hard to soft counts.
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$\begin{figure} \par\includegraphics[angle=-90, width=8.5cm,clip]{5422fig2.ps} \end{figure}$	Figure 2: EPIC spectra of SU Aur (MOS1) and AB Aur (MOS2). Important lines are labeled.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{5422fig3.ps} \end{figure}$	Figure 3: Fluxed, coadded RGS1+RGS2 spectra of SU Aur ( top) and AB Aur ( bottom). The spectra are background subtracted.
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$\begin{figure} \par\includegraphics[width=16.4cm,clip]{5422fig4.ps} \end{figure}$	Figure 4: Data and fitted spectrum of AB Aur (EMD model). The best-fit model is shown by the histograms in the wavelength region used for the fit. For plotting purposes, the MOS2 spectrum has been shifted along the y-axis by 0.001 cts s^-1 Å^-1.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5422f5a.ps}\includegraphics[width=8.2cm,clip]{5422f5b.ps} \end{figure}$	Figure 5: Abundances of AB Aur and SU Aur as a function of FIP. Filled circles: normalized to solar photospheric ratios (Anders & Grevesse 1989; for Fe, Grevesse & Sauval 1999); open circles: normalized to AB Aur photospheric values (Acke & Waelkens 2004).
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$\begin{figure} \par\includegraphics[angle=-90, width=7.8cm,clip]{5422fig6.ps} \end{figure}$	Figure 6: Fit of the O VII triplet using variable electron density. The solid histogram gives the best fit ( $n_{\rm e} < 10^{10}$ cm^-3), while the dotted histogram is for the 90% upper limit to $n_{\rm e}$ ( $n_{\rm e} < 1.3\times 10^{11}$ cm^-3).
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