Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[height=12cm,width=18cm,clip]{INTEGRAL62_Figure_1_IBIS_DU.eps} \end{figure}$ Figure 1: View of the 8 ISGRI MDUs (white color) at the bottom of the passive shield well (black color) after integration in the IBIS detection unit at LABEN premises. Four DBBs (black boxes with a red connector cap) are visible on the shield side (Courtesy IAS).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{INTEGRAL62_Figure_2_polycell.eps} \end{figure}$ Figure 2: Front side of one of the 1024 ISGRI polycells. The 4 $\times$ 4 detectors can be seen in sandwich between the ceramic plates.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{INTEGRAL62_Figure_5_sp_raw.eps} \end{figure}$ Figure 5: Pulse height spectrum acquired at 0 $^\circ$ C with the spare MDU biased at 120 V and illuminated by a ¹³⁹Ce source.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{INTEGRAL62_Figure_6_sp_corr.eps} \end{figure}$ Figure 6: ¹³⁹Ce spectrum corrected for the charge loss. Events with pulse rise-time longer than 4.6 $\mu$ s have been discarded.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{INTEGRAL62_Figure_7_sp_corr_sel.eps} \end{figure}$ Figure 7: ¹³⁹Ce spectrum corrected for the charge loss. Events with pulse rise-time longer than 0.6 $\mu$ s have been discarded.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{INTEGRAL62_Figure_8_ISGRI_spect_perf.eps} \end{figure}$ Figure 8: Spectral performance of ISGRI estimated from MDU 2. Two extreme cases are considered: without any selection on the rise time and with rise time equal to 0.5 $\mu$ s only.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{INTEGRAL62_Figure_9_ISGRI_ARF.eps} \end{figure}$ Figure 9: ISGRI detection efficiency (solid line). The detector efficiency (dashed line), the mask hole transparency (dashed-dotted line) and the polycell cap transparency (dotted line) are also given. Note that since half of the mask elements are opaque, the ISGRI detection efficiency has been divided by a factor two.
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In the text

$\begin{figure} \par\includegraphics[height=12cm,width=18cm,clip]{INTEGRAL62_Figure_1_IBIS_DU.eps} \end{figure}$	Figure 1: View of the 8 ISGRI MDUs (white color) at the bottom of the passive shield well (black color) after integration in the IBIS detection unit at LABEN premises. Four DBBs (black boxes with a red connector cap) are visible on the shield side (Courtesy IAS).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{INTEGRAL62_Figure_2_polycell.eps} \end{figure}$	Figure 2: Front side of one of the 1024 ISGRI polycells. The 4 $\times$ 4 detectors can be seen in sandwich between the ceramic plates.
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$\begin{figure} \par\includegraphics[width=14.8cm,clip]{INTEGRAL62_Figure_3_Cygnus_obs.eps} \end{figure}$	Figure 3: ISGRI image of the Cygnus region in the 15-40 keV energy range.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{INTEGRAL62_Figure_4_bipar.eps} \end{figure}$	Figure 4: Contour plot of the count per pulse-height and pulse rise-time bins.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{INTEGRAL62_Figure_5_sp_raw.eps} \end{figure}$	Figure 5: Pulse height spectrum acquired at 0 $^\circ$ C with the spare MDU biased at 120 V and illuminated by a ¹³⁹Ce source.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{INTEGRAL62_Figure_6_sp_corr.eps} \end{figure}$	Figure 6: ¹³⁹Ce spectrum corrected for the charge loss. Events with pulse rise-time longer than 4.6 $\mu$ s have been discarded.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{INTEGRAL62_Figure_7_sp_corr_sel.eps} \end{figure}$	Figure 7: ¹³⁹Ce spectrum corrected for the charge loss. Events with pulse rise-time longer than 0.6 $\mu$ s have been discarded.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{INTEGRAL62_Figure_8_ISGRI_spect_perf.eps} \end{figure}$	Figure 8: Spectral performance of ISGRI estimated from MDU 2. Two extreme cases are considered: without any selection on the rise time and with rise time equal to 0.5 $\mu$ s only.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{INTEGRAL62_Figure_9_ISGRI_ARF.eps} \end{figure}$	Figure 9: ISGRI detection efficiency (solid line). The detector efficiency (dashed line), the mask hole transparency (dashed-dotted line) and the polycell cap transparency (dotted line) are also given. Note that since half of the mask elements are opaque, the ISGRI detection efficiency has been divided by a factor two.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{INTEGRAL62_Figure_10_ISGRI_BKG.eps} \end{figure}$	Figure 10: ISGRI background spectrum observed while INTEGRAL was pointing to an empty field.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{INTEGRAL62_Figure_11_ISGRI_sensitivity.eps} \end{figure}$	Figure 11: ISGRI broad-band sensitivity.
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