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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{Hc152_f1.ps} \end{figure}$ Figure 1: Significance mosaics (20-100 keV energy band) showing the region around IGR J17285-2922 (indicated by circle). Top left: Mar./Apr. 2003 (A), top right: Aug. 2003 (B), bottom left: Sep./Oct. 2003 (C), bottom right: Feb.-Apr. 2004 (D). The bright source in the bottom right of the frame is the Terzan 2 X-ray source. For mosaic exposures see Table 1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{Hc152_f2.ps} \end{figure}$ Figure 2: Survey light curve for IGR J17285-2922 (20-40 keV energy band). Flux values are averaged over each revolution ( $\sim$ 3 days) for observation sets B and C and averaged over the whole GCDE observation for A and D. The dashed lines represent periods when the source could not be observed by IBIS and the single arrow indicates the revolutions (119 and 120) used for timing and spectral analysis.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.1cm,clip]{Hc152_f3.ps} \end{figure}$ Figure 3: ISGRI light curve of IGR J17285-2922 for revolutions 119 and 120 binned over 8000 s (20-40 keV). Time starts from the beginning of revolution 119, IJD = 1372, where IJD = MJD - 51 544.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.3cm,clip]{Hc152_f4.ps} \end{figure}$ Figure 4: Flux_40-100/Flux_20-40 hardness ratio for revolutions 118 to 121 (bins $\sim$ 3 days). Dotted line shows average hardness for GCDE C.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{Hc152_f5.eps} \end{figure}$ Figure 5: 20-150 keV ISGRI spectrum of IGR J17285-2922 with simple power law model and 3-20 keV JEM-X 3 $\sigma$ upper limits.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{Hc152_f1.ps} \end{figure}$	Figure 1: Significance mosaics (20-100 keV energy band) showing the region around IGR J17285-2922 (indicated by circle). Top left: Mar./Apr. 2003 (A), top right: Aug. 2003 (B), bottom left: Sep./Oct. 2003 (C), bottom right: Feb.-Apr. 2004 (D). The bright source in the bottom right of the frame is the Terzan 2 X-ray source. For mosaic exposures see Table 1.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.1cm,clip]{Hc152_f3.ps} \end{figure}$	Figure 3: ISGRI light curve of IGR J17285-2922 for revolutions 119 and 120 binned over 8000 s (20-40 keV). Time starts from the beginning of revolution 119, IJD = 1372, where IJD = MJD - 51 544.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.3cm,clip]{Hc152_f4.ps} \end{figure}$	Figure 4: Flux_40-100/Flux_20-40 hardness ratio for revolutions 118 to 121 (bins $\sim$ 3 days). Dotted line shows average hardness for GCDE C.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{Hc152_f5.eps} \end{figure}$	Figure 5: 20-150 keV ISGRI spectrum of IGR J17285-2922 with simple power law model and 3-20 keV JEM-X 3 $\sigma$ upper limits.
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