$\begin{figure} \par {\includegraphics[angle=-90,width=8.8cm,clip]{Gj071_f1.ps} } \end{figure}$ Figure 1: Comparison of the PN spectra of 4U 1543-475 with the best-fit power-law model. In the lower panel the residuals (in units of $\sigma$ ) between data and model are shown.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=8.8cm,clip]{Gj071_f2.ps} } \end{figure}$ Figure 2: 3 $\sigma$ upper-limit on the bolometric luminosity of the multi-colour disk as a function of the colour temperature.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=8.8cm,clip]{Gj071_f3.ps} } \end{figure}$ Figure 3: X-ray flux observed by RXTE and XMM-Newton during the 2002 outburst of 4U 1543-475. The open circles refer to the total source flux, the crosses to the power-law component. The last point to the right is our XMM-Newton total flux.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=8.8cm,clip]{Gj071_f1.ps} } \end{figure}$	Figure 1: Comparison of the PN spectra of 4U 1543-475 with the best-fit power-law model. In the lower panel the residuals (in units of $\sigma$ ) between data and model are shown.
Open with DEXTER

$\begin{figure} \par {\includegraphics[angle=-90,width=8.8cm,clip]{Gj071_f2.ps} } \end{figure}$	Figure 2: 3 $\sigma$ upper-limit on the bolometric luminosity of the multi-colour disk as a function of the colour temperature.
Open with DEXTER

$\begin{figure} \par {\includegraphics[angle=-90,width=8.8cm,clip]{Gj071_f3.ps} } \end{figure}$	Figure 3: X-ray flux observed by RXTE and XMM-Newton during the 2002 outburst of 4U 1543-475. The open circles refer to the total source flux, the crosses to the power-law component. The last point to the right is our XMM-Newton total flux.
Open with DEXTER