$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3438fig1.ps}\hspace*{2mm} \includegraphics[angle=-90,width=8.8cm,clip]{3438fig2.ps} \end{figure}$ Figure 1: EPIC pn lightcurves in two energy bands (S, 0.3-2 keV and H, 2-10 keV) and hardness ratios, H/S, during the first ( left) and second observation ( right). Time is in hours of 2003 September 27 (for the first observation) and of the 2003 October 9 (for the second observation). The binning is 64 s.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3438fig3.ps} \end{figure}$ Figure 2: Hardness ratio (H = 2-10 keV; S = 0.3-2 keV counts) versus total intensity (S+H, 0.3-10 keV) for the two pn observations (squares mark the first observation, circles the second). The binning is 512 s.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3438fig4.ps} \end{figure}$ Figure 3: Residuals (in units of standard deviations) when fitting the 2003 September MOS and pn spectra with a single absorbed power-law model. There is a different structure of the residuals in the pn (filled circles), compared with MOS1 (crosses) and MOS2 (triangles). A similar structured excess is present in the 2003 October spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{3438fig5.ps}\hspace*{4mm} ... ...9.ps}\hspace*{4mm} \includegraphics[width=6.2cm,clip]{3438fig10.ps} \end{figure}$ Figure 4: The hydrogen column densities (in units of 10²¹ cm^-2) implied by the optical depths of the Ne, O and Fe edges, from the first ( left) and second observations ( right), depending on the different models assumed for the continua (Table 3). Shadowed regions mark the 90% confidence range for $N_{\rm H}$ resulting from the continuum fits ( VPHABS model, see Table 2).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{3438fig11.ps}\hspace*{3mm} \includegraphics[angle=-90,width=8.7cm,clip]{3438fig12.ps} \end{figure}$ Figure 5: The 0.3-12 keV 4U 1850-087 count spectra (together with the residuals in units of standard deviation) from the two observations (left panel shows the first observation, the right panel the second). The continua have been modeled with a disk-blackbody and a power-law (see Tables 2 and 3 for the continuum and line parameters, respectively).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{3438fig13.ps}\hspace*{3mm} \includegraphics[angle=-90,width=8.7cm,clip]{3438fig14.ps} \end{figure}$ Figure 6: The 0.3-12 keV 4U 1850-087 count spectra (together with the residuals in units of standard deviations) from the two observations (left panel shows the first observation, the right panel the second), fit with the ASCA model with the Ne and O abundances fixed at the values reported in Juett et al. (2001).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3438fig1.ps}\hspace*{2mm} \includegraphics[angle=-90,width=8.8cm,clip]{3438fig2.ps} \end{figure}$	Figure 1: EPIC pn lightcurves in two energy bands (S, 0.3-2 keV and H, 2-10 keV) and hardness ratios, H/S, during the first ( left) and second observation ( right). Time is in hours of 2003 September 27 (for the first observation) and of the 2003 October 9 (for the second observation). The binning is 64 s.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3438fig3.ps} \end{figure}$	Figure 2: Hardness ratio (H = 2-10 keV; S = 0.3-2 keV counts) versus total intensity (S+H, 0.3-10 keV) for the two pn observations (squares mark the first observation, circles the second). The binning is 512 s.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3438fig4.ps} \end{figure}$	Figure 3: Residuals (in units of standard deviations) when fitting the 2003 September MOS and pn spectra with a single absorbed power-law model. There is a different structure of the residuals in the pn (filled circles), compared with MOS1 (crosses) and MOS2 (triangles). A similar structured excess is present in the 2003 October spectrum.
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$\begin{figure} \par\includegraphics[width=6.2cm,clip]{3438fig5.ps}\hspace{4mm} ... ...9.ps}\hspace{4mm} \includegraphics[width=6.2cm,clip]{3438fig10.ps} \end{figure}$	Figure 4: The hydrogen column densities (in units of 10²¹ cm^-2) implied by the optical depths of the Ne, O and Fe edges, from the first ( left) and second observations ( right), depending on the different models assumed for the continua (Table 3). Shadowed regions mark the 90% confidence range for $N_{\rm H}$ resulting from the continuum fits ( VPHABS model, see Table 2).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{3438fig11.ps}\hspace*{3mm} \includegraphics[angle=-90,width=8.7cm,clip]{3438fig12.ps} \end{figure}$	Figure 5: The 0.3-12 keV 4U 1850-087 count spectra (together with the residuals in units of standard deviation) from the two observations (left panel shows the first observation, the right panel the second). The continua have been modeled with a disk-blackbody and a power-law (see Tables 2 and 3 for the continuum and line parameters, respectively).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{3438fig13.ps}\hspace*{3mm} \includegraphics[angle=-90,width=8.7cm,clip]{3438fig14.ps} \end{figure}$	Figure 6: The 0.3-12 keV 4U 1850-087 count spectra (together with the residuals in units of standard deviations) from the two observations (left panel shows the first observation, the right panel the second), fit with the ASCA model with the Ne and O abundances fixed at the values reported in Juett et al. (2001).
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