Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.5cm]{integral74_f1.eps}\end{figure}$ Figure 1: GeD and cold box temperature profile.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm]{integral74_f2.eps}\end{figure}$ Figure 2: Number of GeD per energy resolution interval for the 198 and 1117 keV lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm]{integral74_f3.eps}\end{figure}$ Figure 3: Mean camera (GeD 15 is excluded) energy resolution in the whole energy range one month after launch.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm]{integral74_f4.eps}\end{figure}$ Figure 4: Energy resolution evolution at 1778 keV.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{integral74_f5.eps}\end{figure}$ Figure 5: Temperature profiles during annealing.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{integral74_f6.eps}\end{figure}$ Figure 6: Residuals between measured peak positions and predictedenergy.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{integral74_f7.eps}\end{figure}$ Figure 7: Integral (bottom) and differential (top) spectra for FEE0. Extracted from ACS calibration.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm]{integral74_f8N.eps}\end{figure}$ Figure 8: Tuning of the ACS energy threshold. From left to right: 100 keV untuned, 100 keV tuned, 150 keV tuned, 200 keV tuned, 300 keV tuned. And for comparison again the untuned settingfor: 100 keV, 150 keV, 200 keV, 300 keV and 100 keV.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,angle=0]{integral74_f8.fig9.eps}\end{figure}$ Figure 9: Distribution of the time difference between hits on any neighboring detector pair (i,j) using the first 2 hits of multiple events. The mean misalignment between detector pairs is 10 ns. An association time window of 350 ns has a ME association inefficiency of only 1% for SPI in-flight events (mostly background).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,angle=0]{integral74_f9.eps}\end{figure}$ Figure 10: Distribution of the difference $\Delta t=t({\rm ACS})-t({\rm Ge})$ between the arrival time of an ACS time-tag and a time-tag from any of the 19 Ge detectors (top graph). The signals are well aligned in time: all non-accidental hits show $\Delta t<0$ , meaning that the ACS trigger arrives before the Ge detector time-tag. The ACS gate width is well set to 750 ns: all non-accidental hits have $\vert\Delta t\vert<750$ ns, even considering the time-tags at the extreme of the energy range: middle and bottom graphs. This width is kept as low as possible for a low ACS dead-time (8% with this setting).
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In the text

$\begin{figure} \par\includegraphics[width=6cm,angle=0]{integral74_f10.eps}\end{figure}$ Figure 11: Distribution of the non saturating, non vetoed Ge counts on the SPI camera (vertical axis in counts/s, Ysi and Zsi axis = positions of the detectors in mm, detector numbers marked on the plot). The outer detectors show less counts, since Compton scattered photons may escape into the BGO shield and activate a veto signal, which suppresses the event (self-veto effect).
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,angle=0]{integral74_f11.eps} \par\end{figure}$ Figure 12: Count rates observed for GeDs 0 to 18 for: all counts below 8 MeV (top graph); saturating events (energies greater than 8 MeV, middle graph); and non vetoed counts below 8 MeV (bottom graph).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,angle=0]{integral74_f12.eps}\end{figure}$ Figure 13: Evolution of the SPI telemetry allocation with time and corresponding data losses.
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,angle=0]{integral74_f13.eps}\end{figure}$ Figure 14: Image of the Crab Nebula in the 20-50 keV energy range, the scale is logarithmic.
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In the text

$\begin{figure} \par\includegraphics[width=17.0cm,angle=0]{integral74_f14.eps}\end{figure}$ Figure 15: Image of the Galactic plane obtained during the Galactic Center Deep Exposure 20-50 keV.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,angle=0]{integral74_f15.ps}\end{figure}$ Figure 16: Spectrum of the Crab nebula.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm]{integral74_f16.eps}\end{figure}$ Figure 17: Continuum sensitivity for on-axis point source and for 10⁶ s observation time.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm]{integral74_f17.eps}\par\end{figure}$ Figure 18: 3 $\sigma$ narrow line sensitivity for 10⁶ s observation time.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{integral74_f1.eps}\end{figure}$	Figure 1: GeD and cold box temperature profile.
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$\begin{figure} \par\includegraphics[width=8.2cm]{integral74_f2.eps}\end{figure}$	Figure 2: Number of GeD per energy resolution interval for the 198 and 1117 keV lines.
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$\begin{figure} \par\includegraphics[width=8.4cm]{integral74_f3.eps}\end{figure}$	Figure 3: Mean camera (GeD 15 is excluded) energy resolution in the whole energy range one month after launch.
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$\begin{figure} \par\includegraphics[width=8.3cm]{integral74_f4.eps}\end{figure}$	Figure 4: Energy resolution evolution at 1778 keV.
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$\begin{figure} \par\includegraphics[width=8.5cm]{integral74_f5.eps}\end{figure}$	Figure 5: Temperature profiles during annealing.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{integral74_f6.eps}\end{figure}$	Figure 6: Residuals between measured peak positions and predictedenergy.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{integral74_f7.eps}\end{figure}$	Figure 7: Integral (bottom) and differential (top) spectra for FEE0. Extracted from ACS calibration.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm]{integral74_f8N.eps}\end{figure}$	Figure 8: Tuning of the ACS energy threshold. From left to right: 100 keV untuned, 100 keV tuned, 150 keV tuned, 200 keV tuned, 300 keV tuned. And for comparison again the untuned settingfor: 100 keV, 150 keV, 200 keV, 300 keV and 100 keV.
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$\begin{figure} \par\includegraphics[width=8.8cm,angle=0]{integral74_f8.fig9.eps}\end{figure}$	Figure 9: Distribution of the time difference between hits on any neighboring detector pair (i,j) using the first 2 hits of multiple events. The mean misalignment between detector pairs is 10 ns. An association time window of 350 ns has a ME association inefficiency of only 1% for SPI in-flight events (mostly background).
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$\begin{figure} \par\includegraphics[width=6cm,angle=0]{integral74_f10.eps}\end{figure}$	Figure 11: Distribution of the non saturating, non vetoed Ge counts on the SPI camera (vertical axis in counts/s, Ysi and Zsi axis = positions of the detectors in mm, detector numbers marked on the plot). The outer detectors show less counts, since Compton scattered photons may escape into the BGO shield and activate a veto signal, which suppresses the event (self-veto effect).
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$\begin{figure} \par\includegraphics[width=8.7cm,angle=0]{integral74_f11.eps} \par\end{figure}$	Figure 12: Count rates observed for GeDs 0 to 18 for: all counts below 8 MeV (top graph); saturating events (energies greater than 8 MeV, middle graph); and non vetoed counts below 8 MeV (bottom graph).
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$\begin{figure} \par\includegraphics[width=8.8cm,angle=0]{integral74_f12.eps}\end{figure}$	Figure 13: Evolution of the SPI telemetry allocation with time and corresponding data losses.
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$\begin{figure} \par\includegraphics[width=8.0cm,angle=0]{integral74_f13.eps}\end{figure}$	Figure 14: Image of the Crab Nebula in the 20-50 keV energy range, the scale is logarithmic.
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$\begin{figure} \par\includegraphics[width=17.0cm,angle=0]{integral74_f14.eps}\end{figure}$	Figure 15: Image of the Galactic plane obtained during the Galactic Center Deep Exposure 20-50 keV.
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$\begin{figure} \par\includegraphics[width=8.4cm,angle=0]{integral74_f15.ps}\end{figure}$	Figure 16: Spectrum of the Crab nebula.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm]{integral74_f16.eps}\end{figure}$	Figure 17: Continuum sensitivity for on-axis point source and for 10⁶ s observation time.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm]{integral74_f17.eps}\par\end{figure}$	Figure 18: 3 $\sigma$ narrow line sensitivity for 10⁶ s observation time.
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