All Figures

$\begin{figure} \par\includegraphics[height=17.5cm,angle=90,clip]{0940fig1.ps} \end{figure}$ Figure 1: 2003 September 11 EPIC-pn ( left) and OM B filter ( right) images of the area around the 2 $^\prime$ INTEGRAL uncertainty region for IGR J17544-2619 of Sunyaev et al. (2003, big circle). The contours shown in the optical image correspond to the EPIC-pn image (0.005, 0.010, 0.015, 0.020 and 0.025 counts s^-1), which clearly excludes 1RXS J175428.3-262035 (small circle).
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=8.5cm,clip]{0940fg2a.p... ...m} \includegraphics[angle=-90,width=8.5cm,clip]{0940fg2b.ps} } \end{figure}$ Figure 2: IGR J17544-2619 0.5-10 keV light curves for the September 11 (pn; lower left) and September 17, 2003 (MOS1; lower right) observations with integration times of 50 s. A MOS1 count rate of 1 count s^-1 corresponds to $\sim$ 3.5 pn count s^-1 (see text). The upper panels show the hardness ratio (counts between 2-10 keV divided by those between 0.5-2 keV) with a 200 s binning.
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In the text

$\begin{figure} \par\includegraphics[height=8.5cm,angle=-90,clip]{0940fig3.ps} \end{figure}$ Figure 3: Enlarged view of the 2-10 keV September 17 light curve showing a number of short flares that took place between 17:45 and 18:15 UTC (binning is 10 s).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0940fig4.ps} \end{figure}$ Figure 4: Time selected (see text) pn count spectra from the September 11, 2003 observation. From bottom to top the 3 spectra correspond to pre-flare, post-flare and flaring intervals. The best-fit absorbed power-law models with the same value of $\alpha$ and different values of the normalisation and $N{\rm _H}$ for each spectrum are shown as histograms.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0940fig5.ps} \end{figure}$ Figure 5: Time selected MOS1 count spectra from the September 17, 2003 observation. The upper spectrum is from intervals when the 0.5-10 keV count rate was >2.5 s^-1, the lower one from intervals below this value. The best-fit absorbed power-law models with the same value of $\alpha$ and different values of the normalisation and $N{\rm _H}$ for each spectrum are shown as histograms.
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In the text

$\begin{figure} \par\includegraphics[height=17.5cm,angle=90,clip]{0940fig1.ps} \end{figure}$	Figure 1: 2003 September 11 EPIC-pn ( left) and OM B filter ( right) images of the area around the 2 $^\prime$ INTEGRAL uncertainty region for IGR J17544-2619 of Sunyaev et al. (2003, big circle). The contours shown in the optical image correspond to the EPIC-pn image (0.005, 0.010, 0.015, 0.020 and 0.025 counts s^-1), which clearly excludes 1RXS J175428.3-262035 (small circle).
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$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=8.5cm,clip]{0940fg2a.p... ...m} \includegraphics[angle=-90,width=8.5cm,clip]{0940fg2b.ps} } \end{figure}$	Figure 2: IGR J17544-2619 0.5-10 keV light curves for the September 11 (pn; lower left) and September 17, 2003 (MOS1; lower right) observations with integration times of 50 s. A MOS1 count rate of 1 count s^-1 corresponds to $\sim$ 3.5 pn count s^-1 (see text). The upper panels show the hardness ratio (counts between 2-10 keV divided by those between 0.5-2 keV) with a 200 s binning.
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$\begin{figure} \par\includegraphics[height=8.5cm,angle=-90,clip]{0940fig3.ps} \end{figure}$	Figure 3: Enlarged view of the 2-10 keV September 17 light curve showing a number of short flares that took place between 17:45 and 18:15 UTC (binning is 10 s).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0940fig4.ps} \end{figure}$	Figure 4: Time selected (see text) pn count spectra from the September 11, 2003 observation. From bottom to top the 3 spectra correspond to pre-flare, post-flare and flaring intervals. The best-fit absorbed power-law models with the same value of $\alpha$ and different values of the normalisation and $N{\rm _H}$ for each spectrum are shown as histograms.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0940fig5.ps} \end{figure}$	Figure 5: Time selected MOS1 count spectra from the September 17, 2003 observation. The upper spectrum is from intervals when the 0.5-10 keV count rate was >2.5 s^-1, the lower one from intervals below this value. The best-fit absorbed power-law models with the same value of $\alpha$ and different values of the normalisation and $N{\rm _H}$ for each spectrum are shown as histograms.
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