Astronomy & Astrophysics

All Figures

$\begin{figure} \par\epsfig{file=INTEGRAL25_FWHM.eps,width=8.8cm} \end{figure}$ Figure 1: Spectral resolution ( ${\it FWHM}$ ) for the flight model camera at 90 K. For each energy, the resolutions for the 19 individual detectors are plotted. The fit function is given by Eq. (2).
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In the text

$\begin{figure} \par\epsfig{file=INTEGRAL25_EffSE.eps,width=8.8cm} \end{figure}$ Figure 2: Full-energy peak efficiency for sources on the SPI optical axis ( $\alpha =0^\circ$ ), without mask. An average for detectors 1 to 18 is shown; detector 0 is plotted separately (see Sect. 5.2). The measurements are compared to Monte-Carlo simulations.
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In the text

$\begin{figure} \par\mbox{ \epsfig{figure=INTEGRAL25_All0.eps,width=8.75cm}\hspace*{1mm} \epsfig{figure=INTEGRAL25_All8.eps,width=8.75cm} } \par\end{figure}$ Figure 3: For each detector, a plot of the efficiency versus energy is shown (in each plot, the line energy increases from left to right according to the 14 energies used). The crosses represent the mass of the crystal. When the detector is not shadowed, the efficiency depends mainly on its mass. Left panel: at $0^\circ$ , source on axis, the detectors 0, 2 and 3 are partially shadowed by the PSAC-alignment device. Right panel: when the source is at $8^\circ$ , detectors 16 to 18 are shadowed by the ACS. The alignment device is projected outside the detection plane.
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In the text

$\begin{figure} \par\epsfig{figure=INTEGRAL25_EffMESE.eps,width=8.75cm} \end{figure}$ Figure 4: Full-energy peak efficiency for SE, ME and all events (SE+ME) and for ME with multiplicity m = 2, 3 and >3, for the camera without mask. The effective area is the geometric area multiplied by the efficiency.
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In the text

$\begin{figure} \par\epsfig{figure=INTEGRAL25_BLC2PLGC03,width=8.75cm,height=6.5cm} \end{figure}$ Figure 5: The on-axis, full-energy peak efficiencies of detector 0 and 3 for SPI with its mask. The data are: 8 m BLC data without mask corrected for the mask absorption ( $\cdot$ ), 125 m BLC data with mask, ( $\circ$ ) and 8 m ESTEC data with mask ( $\times$ ). For detector 0, the disagreement between the curves shows the difficulty of alignment device modelisation.
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In the text

$\begin{figure} \par\epsfig{file=INTEGRAL25_EffSEMEARF2.eps,width=8.8cm} \end{figure}$ Figure 6: Full-energy peak effective area of SPI telescope using all events (SE+ME). This curve is representative of the in flight effective area for an on-axis source. We compare it to the response matrix before the launch (release 1, Nov. 2002) and after the launch (release 3, July 2003).
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In the text

$\begin{figure} \par\psfig{figure=INTEGRAL25_psfs_4_col.ps,width=6.4cm,angle=-90} \end{figure}$ Figure 7: The PSF determined from measurements of 4 different sources at 125 m. Each curve is the mean of cross-sections through the response in two orthogonal directions; a background level has been subtracted from each and the curves normalized to the same peak height. The mean FWHM is 2.55 $^\circ$ . (²⁴¹Am: 60 keV; ¹³⁷Cs: 662 keV; ⁶⁰Co: 1332 keV; ²⁴Na: 2754 keV).
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In the text

$\begin{figure} \par\psfig{figure=INTEGRAL25_fig_pos.ps,width=5cm,height=8cm,angle=-90} \end{figure}$ Figure 8: The error in the determination of a narrow line source position from analysis of calibration data. Squares: subsets of data, circles: mean of 10-20 trials with samples of random noise added. Open symbols: deviations from the nominal position, filled symbols: deviations from an assumed displaced source position. The line corresponds to 2.5 $^\circ$ $/N_\sigma$ .
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In the text

$\begin{figure} \par\psfig{figure=INTEGRAL25_source_sep.ps,width=8.8cm} \end{figure}$ Figure 9: Maximum entropy image in the 1173 keV ⁶⁰Co line shows the capability of the instrument to separate sources closer than the angular resolution, where the signal-to-noise ratio is good. The sources are separated by 1 $^\circ$ .
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In the text

$\begin{figure} \par\epsfig{file=INTEGRAL25_seuils.eps,width=8.8cm,height=4.5cm} \end{figure}$ Figure 10: For PMT₁(solid), $E_{\rm th}$ = 100 keV and $a = \sqrt {50}$ , for PMT₂(open), 120 keV and $\sqrt {10}$ . These curves illustrate the large differences between ACS crystals and PMTs combinations.
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In the text

$\begin{figure} \par\epsfig{file=INTEGRAL25_ACS.eps,width=8.8cm}\par\end{figure}$ Figure 11: ACS permeability as a function of the angle from the axis (BLC, ¹³⁷Cs source)
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In the text

$\begin{figure} \par\epsfig{file=INTEGRAL25_FWHM.eps,width=8.8cm} \end{figure}$	Figure 1: Spectral resolution ( ${\it FWHM}$ ) for the flight model camera at 90 K. For each energy, the resolutions for the 19 individual detectors are plotted. The fit function is given by Eq. (2).
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$\begin{figure} \par\epsfig{file=INTEGRAL25_EffSE.eps,width=8.8cm} \end{figure}$	Figure 2: Full-energy peak efficiency for sources on the SPI optical axis ( $\alpha =0^\circ$ ), without mask. An average for detectors 1 to 18 is shown; detector 0 is plotted separately (see Sect. 5.2). The measurements are compared to Monte-Carlo simulations.
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$\begin{figure} \par\epsfig{figure=INTEGRAL25_EffMESE.eps,width=8.75cm} \end{figure}$	Figure 4: Full-energy peak efficiency for SE, ME and all events (SE+ME) and for ME with multiplicity m = 2, 3 and >3, for the camera without mask. The effective area is the geometric area multiplied by the efficiency.
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$\begin{figure} \par\epsfig{figure=INTEGRAL25_BLC2PLGC03,width=8.75cm,height=6.5cm} \end{figure}$	Figure 5: The on-axis, full-energy peak efficiencies of detector 0 and 3 for SPI with its mask. The data are: 8 m BLC data without mask corrected for the mask absorption ( $\cdot$ ), 125 m BLC data with mask, ( $\circ$ ) and 8 m ESTEC data with mask ( $\times$ ). For detector 0, the disagreement between the curves shows the difficulty of alignment device modelisation.
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$\begin{figure} \par\epsfig{file=INTEGRAL25_EffSEMEARF2.eps,width=8.8cm} \end{figure}$	Figure 6: Full-energy peak effective area of SPI telescope using all events (SE+ME). This curve is representative of the in flight effective area for an on-axis source. We compare it to the response matrix before the launch (release 1, Nov. 2002) and after the launch (release 3, July 2003).
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$\begin{figure} \par\psfig{figure=INTEGRAL25_psfs_4_col.ps,width=6.4cm,angle=-90} \end{figure}$	Figure 7: The PSF determined from measurements of 4 different sources at 125 m. Each curve is the mean of cross-sections through the response in two orthogonal directions; a background level has been subtracted from each and the curves normalized to the same peak height. The mean FWHM is 2.55 $^\circ$ . (²⁴¹Am: 60 keV; ¹³⁷Cs: 662 keV; ⁶⁰Co: 1332 keV; ²⁴Na: 2754 keV).
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$\begin{figure} \par\psfig{figure=INTEGRAL25_fig_pos.ps,width=5cm,height=8cm,angle=-90} \end{figure}$	Figure 8: The error in the determination of a narrow line source position from analysis of calibration data. Squares: subsets of data, circles: mean of 10-20 trials with samples of random noise added. Open symbols: deviations from the nominal position, filled symbols: deviations from an assumed displaced source position. The line corresponds to 2.5 $^\circ$ $/N_\sigma$ .
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$\begin{figure} \par\psfig{figure=INTEGRAL25_source_sep.ps,width=8.8cm} \end{figure}$	Figure 9: Maximum entropy image in the 1173 keV ⁶⁰Co line shows the capability of the instrument to separate sources closer than the angular resolution, where the signal-to-noise ratio is good. The sources are separated by 1 $^\circ$ .
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$\begin{figure} \par\epsfig{file=INTEGRAL25_seuils.eps,width=8.8cm,height=4.5cm} \end{figure}$	Figure 10: For PMT₁(solid), $E_{\rm th}$ = 100 keV and $a = \sqrt {50}$ , for PMT₂(open), 120 keV and $\sqrt {10}$ . These curves illustrate the large differences between ACS crystals and PMTs combinations.
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$\begin{figure} \par\epsfig{file=INTEGRAL25_ACS.eps,width=8.8cm}\par\end{figure}$	Figure 11: ACS permeability as a function of the angle from the axis (BLC, ¹³⁷Cs source)
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