All Figures

$\begin{figure} \par\psfig{figure=werner_f1.ps,width=8.8cm,clip=t} \end{figure}$ Figure 1: The PCA lightcurve of the SAX J1747.0-2853 obtained between 1999 February 6 and 2003 March 30. The times of the five BeppoSAX NFI observations are indicated by the horizontal line and the observations with XMM-Newton and Chandra are indicated by the vertical dashed lines.
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In the text

$\begin{figure} \par\psfig{figure=werner_f2.ps,width=8.8cm,clip=t} \end{figure}$ Figure 2: The PCA lightcurve of the SAX J1747.0-2853 obtained between 2000 February 10 and October 30. The five BeppoSAX NFI observations and the later XMM-Newton observation are indicated.
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In the text

$\begin{figure} \par\psfig{figure=werner_f3.ps,width=8.8cm,clip=t,angle=270.} \end{figure}$ Figure 3: MECS (1.8-10 keV) and PDS (15-200 keV) spectra of SAX J1747.0-2853 from 2000 March 13 ( $1{\rm st}$ from the top), March 16 ( $2{\rm nd}$ from the top), March 27 ( $3{\rm rd}$ from the top) April 7 ( $1{\rm st}$ from the bottom) and April 12 (2nd from the bottom). The MECS spectra are illustrating well the changes of the brightness of the source and the changes of the shape of the spectra. The small changes in the PDS spectra are indicative of contamination by other sources. Only the PDS data from the first observation are somewhat above the noise level created by other sources in the field of view of the PDS.
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In the text

$\begin{figure} \par\psfig{figure=werner_f4.ps,width=8.8cm,clip=t,angle=270.} \end{figure}$ Figure 4: Spectrum of the SAX J1747.0-2853 obtained during the observation on 2000 April 7, when the source was in the minimum between the two peaks. The spectrum is fitted with Comptonization, disk blackbody and a narrow line, all with absorption. The equivalent width of the iron line at this observation is the highest of all observations.
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In the text

$\begin{figure} \par\psfig{figure=werner_f5.ps,width=8.8cm,clip=t,angle=270.} \end{figure}$ Figure 5: Spectrum of the SAX J1747.0-2853 obtained by the XMM-Newton EPIC cameras during the observation on 2000 September 21, with the best fit and 1 $\sigma$ residuals. The spectrum is fitted as the sum of a disk blackbody and a Comptonized component all with absorption. The upper curve shows the data obtained by the EPIC-pn, the lower curves show the MOS1 and MOS2 data.
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In the text

$\begin{figure} \par\psfig{figure=werner_f6.ps,width=8.5cm,clip=t} \end{figure}$ Figure 6: The PCA lightcurve of SAX J1747.0-2853 with the times (as indicated by horizontal lines) when the BeppoSAX WFC had the source in its field of view with sufficient sensitivity, and with the times of the detected X-ray bursts (as indicated by vertical dotted lines; this includes the four NFI and ASCA detected bursts). The number of the detected X-ray bursts in an observation window is indicated over the horizontal lines.
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In the text

$\begin{figure} \par\psfig{figure=werner_f1.ps,width=8.8cm,clip=t} \end{figure}$	Figure 1: The PCA lightcurve of the SAX J1747.0-2853 obtained between 1999 February 6 and 2003 March 30. The times of the five BeppoSAX NFI observations are indicated by the horizontal line and the observations with XMM-Newton and Chandra are indicated by the vertical dashed lines.
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$\begin{figure} \par\psfig{figure=werner_f2.ps,width=8.8cm,clip=t} \end{figure}$	Figure 2: The PCA lightcurve of the SAX J1747.0-2853 obtained between 2000 February 10 and October 30. The five BeppoSAX NFI observations and the later XMM-Newton observation are indicated.
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$\begin{figure} \par\psfig{figure=werner_f4.ps,width=8.8cm,clip=t,angle=270.} \end{figure}$	Figure 4: Spectrum of the SAX J1747.0-2853 obtained during the observation on 2000 April 7, when the source was in the minimum between the two peaks. The spectrum is fitted with Comptonization, disk blackbody and a narrow line, all with absorption. The equivalent width of the iron line at this observation is the highest of all observations.
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$\begin{figure} \par\psfig{figure=werner_f5.ps,width=8.8cm,clip=t,angle=270.} \end{figure}$	Figure 5: Spectrum of the SAX J1747.0-2853 obtained by the XMM-Newton EPIC cameras during the observation on 2000 September 21, with the best fit and 1 $\sigma$ residuals. The spectrum is fitted as the sum of a disk blackbody and a Comptonized component all with absorption. The upper curve shows the data obtained by the EPIC-pn, the lower curves show the MOS1 and MOS2 data.
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