All Figures

$\begin{figure} \par\includegraphics[height=8.6cm,width=7.14cm,angle=-90,clip]{15... ...udegraphics[height=8.6cm,width=7.14cm,angle=-90,clip]{1567_fig2.ps} \end{figure}$ Figure 1: MECS 1.8-10 keV light curves of the first ( upper panel) and second ( lower panel) observation of GX 17+2. The bin size in both cases is 100 s. Time is given in seconds from the beginning of each observation (see Table 1).
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In the text

$\begin{figure} { \epsfig{figure=1567_fig3.ps, height=6.5cm, width=6.5cm}\hspace*{2mm} \epsfig{figure=1567_fig4.ps, height=6.5cm, width=6.5cm} }\end{figure}$ Figure 2: Left panel: HID of the two BeppoSAX observations of GX 17+2. Diamonds: first observation. Open squares: second observation. The four count-rate regions are also shown. Each point corresponds to a bin size of 100 s. Right panel: source HID of both our observations (same symbols as in the left panel) and that performed by DS2000 ( crosses). The bin size of the 1997 October data points is 400 s. A typical error bar is shown on the top right of each panel.
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In the text

$\begin{figure} { \epsfig{figure=1567_fig5.ps, height=6.5cm, width=6.5cm, angle=-... ...psfig{figure=1567_fig6.ps, height=6.5cm, width=6.5cm, angle=-90} }\end{figure}$ Figure 3: Count-rate spectra of the first observation ( left panel) and of the second observation ( right panel) of GX 17+2 and best-fit folded model WABS( BB + COMPTT + Gaussian) with $kT_{\rm bb}< kT_{\rm s}$ . In the first observation, an absorption edge was also included. Below each panel are shown the residuals to the model in units of $\sigma$ . The last two PDS points of the second observation have ${\it S/N} < 3$ , so they were not included in the fit and are reported as 2 $\sigma$ upper limits. Similar results are obtained for the same model but with $kT_{\rm bb}> kT_{\rm s}$ .
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In the text

$\begin{figure} { \epsfig{figure=1567_fig7.ps, height=7cm, width=3cm, angle=-90}\... ...} \epsfig{figure=1567_fig8.ps, height=7cm, width=3cm, angle=-90} }\end{figure}$ Figure 4: Residuals in units of $\sigma$ to the model WABS( BB + EQPAIR + Gaussian), assuming purely thermal Comptonization, for the first ( left panel) and for second ( right panel) observation of GX 17+2.
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In the text

$\begin{figure} { \epsfig{figure=1567_fig9.ps , width=6.5cm, height=6.5cm}\hspace*{2mm} \epsfig{figure=1567_fig10.ps , width=6.5cm, height=6.5cm} }\end{figure}$ Figure 5: Unabsorbed EF(E) spectrum of the first ( left panel) and of the second ( right panel) observation of GX 17+2 along with the best-fit model WABS( BB + EQPAIR + Gaussian). A hybrid spectrum of the Comptonizing electrons is assumed. The 2 $\sigma$ upper limit of the last two PDS points of the second observation is also reported. Below each panel, the residuals between the data and the model in units of $\sigma$ are shown. Different line styles represent the single components. Dotted: BB. Dotted-dashed: EQPAIR. Dashed: Gaussian emission line.
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In the text

$\begin{figure} \par\includegraphics[height=8.6cm,width=7.14cm,angle=-90,clip]{15... ...udegraphics[height=8.6cm,width=7.14cm,angle=-90,clip]{1567_fig2.ps} \end{figure}$	Figure 1: MECS 1.8-10 keV light curves of the first ( upper panel) and second ( lower panel) observation of GX 17+2. The bin size in both cases is 100 s. Time is given in seconds from the beginning of each observation (see Table 1).
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$\begin{figure} { \epsfig{figure=1567_fig7.ps, height=7cm, width=3cm, angle=-90}\... ...} \epsfig{figure=1567_fig8.ps, height=7cm, width=3cm, angle=-90} }\end{figure}$	Figure 4: Residuals in units of $\sigma$ to the model WABS( BB + EQPAIR + Gaussian), assuming purely thermal Comptonization, for the first ( left panel) and for second ( right panel) observation of GX 17+2.
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