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$\begin{figure} \par\includegraphics[width=14.4cm,clip]{newimagebw.ps} \end{figure}$ Figure 1: Images of a 4 $^{\circ }\times 3^{\circ }$ region containing the position of SGR 1806-20 obtained with the IBIS/ISGRI instrument in the 20-60 keV ( left) and 60-100 keV energy range ( right). The other detected sources are (1) GX 9+1, (2) IGR J18027-2016 (Revnivtsev et al. 2004), and (3) IGR J17597-2201 (Lutovinov et al. 2003).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{spectranew.ps} \end{figure}$ Figure 2: IBIS/ISGRI spectra of SGR 1806-20: a) persistent emission March 2003-Apr. 2004, b) persistent emission Sept.-Oct. 2004, c) one burst (scaled down by a factor 10⁴). The solid lines are the best fits (power laws in a) and b), thermal bremsstrahlung in c)). The dashed lines indicate the extrapolation of power-law spectra measured in the 1-10 keV range with XMM-Newton (Mereghetti et al. 2004b).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{2plot.ps} \end{figure}$ Figure 3: a) histogram of number of bursts per day detected by the third Interplanetary Network (IPN). This histogram includes mostly those bursts with fluences larger than 10^-7 erg cm^-2 and is not corrected for experiment duty cycles and source visibility. It therefore represents only the trend of the burst rate and not its true value. b) Count rate in the 20-60 keV range. The horizontal error bars indicate the time spanned by the (non continuous) observations.
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In the text

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{newimagebw.ps} \end{figure}$	Figure 1: Images of a 4 $^{\circ }\times 3^{\circ }$ region containing the position of SGR 1806-20 obtained with the IBIS/ISGRI instrument in the 20-60 keV ( left) and 60-100 keV energy range ( right). The other detected sources are (1) GX 9+1, (2) IGR J18027-2016 (Revnivtsev et al. 2004), and (3) IGR J17597-2201 (Lutovinov et al. 2003).
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