Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5157fig1.eps} \end{figure}$ Figure 1: IBIS /ISGRI significance image of the Coma cluster in the 18-30 $\ensuremath {{\rm keV}}$ energy range. The black cross indicates the position of NGC 4874, near the center of the X-ray emission from Coma (Briel et al. 2001). The white cross shows the location of X Comae, a bright Seyfert galaxy at $\sim$ 30 $^{\prime }$ from the cluster. The colour scale is linear, with black corresponding to 1 $\sigma$ and white to 8 $\sigma$ . The IBIS SPSF is also shown in the lower right corner.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{5157fig2a.eps}\par\includegraphics[width=7.5cm,clip]{5157fig2b.eps} \end{figure}$ Figure 2: Top panel: XMM-Newton 0.3-2 $\ensuremath {{\rm keV}}$ mosaic image Neumann et al. (2003) with IBIS /ISGRI significance contours in the 18-30 $\ensuremath {{\rm keV}}$ energy range, going from 2 $\sigma$ to 10 $\sigma$ . Bottom panel: IBIS /ISGRI image of flux per pixel in the 18-30 $\ensuremath {{\rm keV}}$ band centered on the Coma Cluster ( left), the predicted morphology based on the XMM-Newton images in intensity and inferred temperature ( middle), and the correlation between the 18-30 $\ensuremath {{\rm keV}}$ and 0.3-2 $\ensuremath {{\rm keV}}$ images ( right). The white squares delineate the regions over which the flux was summed for the purpose of correlation study.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5157fig3.eps} \end{figure}$ Figure 3: The 18-30 $\ensuremath {{\rm keV}}$ IBIS /ISGRI integrated intensity (left scale, solid line with error bars) and corresponding significance calculated on concentric circles and expressed as a function of radius (right scale, dashed line). The shaded area shows the intensity within the 1 $\sigma$ error derived from RXTE observations (Rephaeli & Gruber 2002; Rossetti & Molendi 2004).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{5157fig4.eps} \end{figure}$ Figure 4: IBIS /ISGRI spectrum of the Coma Cluster . The upper limit in the 30-50 $\ensuremath {{\rm keV}}$ range is calculated assuming that the source has the same shape as it does in the 18-30 $\ensuremath {{\rm keV}}$ energy range. At higher energies, the upper limits are derived as for a point-source. The best-fit RXTE spectrum within its 1 $\sigma$ uncertainties, is shown as the dashed area. Upper limits are given at the 3 $\sigma$ confidence level.
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In the text