Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[width=5.2cm,clip]{INTEGRAL18_f1.eps} \end{figure}$ Figure 1: Principle of IBIS OBCU operation: photons emitted towards the IBIS detector planes are "tagged'' by simultaneous detections in the BGO tagging system.
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In the text

$\begin{figure} \par\includegraphics[width=13.7cm,clip]{INTEGRAL18_f2.eps} \end{figure}$ Figure 2: Internal diagnostic pulse height spectra from the OBCU for (left) in-flight operation and (right) during ground calibrations. The individual Gaussian fits to the 511, 1275 and 1786 lines, together with an exponential background component, are shown together with the recorded spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{INTEGRAL18_f3.eps} \end{figure}$ Figure 3: Proposed saturation, blinding and baseline restoration effects in OBCU electronics due to the detection of high energy photons or charged particles.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{INTEGRAL18_f4.eps} \end{figure}$ Figure 4: Typical S2 (ISGRI calibration) spectrum summed over all pixels. PHA values have been gain-normalised, but charge loss correction has not been applied.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{INTEGRAL18_f5.eps} \end{figure}$ Figure 5: Typical S5 (PICSIT calibration) spectrum, summed over all pixels and integrated for one revolution.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{INTEGRAL18_f6.eps} \end{figure}$ Figure 6: Distribution of detected calibration photons across the PICsIT detector plane. The non-uniform distribution derives from a combination of source flux, detection efficiency and tagging efficiency. Note the presence of a few permanently off pixels.
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm,clip]{INTEGRAL18_f1.eps} \end{figure}$	Figure 1: Principle of IBIS OBCU operation: photons emitted towards the IBIS detector planes are "tagged'' by simultaneous detections in the BGO tagging system.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=13.7cm,clip]{INTEGRAL18_f2.eps} \end{figure}$	Figure 2: Internal diagnostic pulse height spectra from the OBCU for (left) in-flight operation and (right) during ground calibrations. The individual Gaussian fits to the 511, 1275 and 1786 lines, together with an exponential background component, are shown together with the recorded spectrum.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{INTEGRAL18_f3.eps} \end{figure}$	Figure 3: Proposed saturation, blinding and baseline restoration effects in OBCU electronics due to the detection of high energy photons or charged particles.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{INTEGRAL18_f4.eps} \end{figure}$	Figure 4: Typical S2 (ISGRI calibration) spectrum summed over all pixels. PHA values have been gain-normalised, but charge loss correction has not been applied.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{INTEGRAL18_f5.eps} \end{figure}$	Figure 5: Typical S5 (PICSIT calibration) spectrum, summed over all pixels and integrated for one revolution.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{INTEGRAL18_f6.eps} \end{figure}$	Figure 6: Distribution of detected calibration photons across the PICsIT detector plane. The non-uniform distribution derives from a combination of source flux, detection efficiency and tagging efficiency. Note the presence of a few permanently off pixels.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{INTEGRAL18_f7.ps} \end{figure}$	Figure 7: Spatial variation of tagging efficiency derived from GEANT4 simulations.
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