Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[scale=0.4,clip]{integral35_f1.ps} \end{figure}$ Figure 1: PICsIT in-orbit background spectrum for single and multiple events compared with the expected expected spectrum obtained from MonteCarlo simulations normalized to 7500 counts/s.
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In the text

$\begin{figure} \par\mbox{\includegraphics[scale=0.45,clip]{integral35_f2a.ps} \includegraphics[scale=0.45,clip]{integral35_f2b.ps} } \end{figure}$ Figure 2: PICsIT minimum detectable flux for continuum (left panel) and narrow line (right panel) emission as a function of energy assuming only statistical effects, and the in-flight measured background. The dashed lines of the first two bins in the left panel indicate the worsening due to the effect of cosmic-ray induced tracks.
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In the text

$\begin{figure} \par\mbox{\includegraphics[scale=0.24,clip]{integral35_f3a.eps} \... ...f3c.eps} \includegraphics[scale=0.24,clip]{integral35_f3d.eps} } \end{figure}$ Figure 3: Crab significance images and profiles obtained from observations performed during revolution 43 with the standard ISDC/ISSW. Deconvolved images are shown for 4 energy bands: 203-252 keV, 252-329 keV, 329-455 keV, 455-655 keV.
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In the text

$\begin{figure} \par\includegraphics[scale=0.28,clip]{integral35_f4.eps} \end{figure}$ Figure 4: Cyg X-1 significance image and profile in the 252-329 keV band obtained from a 80 ks observation in revolution 11.
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In the text

$\begin{figure} \par\includegraphics[scale=0.4,clip]{integral35_f1.ps} \end{figure}$	Figure 1: PICsIT in-orbit background spectrum for single and multiple events compared with the expected expected spectrum obtained from MonteCarlo simulations normalized to 7500 counts/s.
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$\begin{figure} \par\mbox{\includegraphics[scale=0.45,clip]{integral35_f2a.ps} \includegraphics[scale=0.45,clip]{integral35_f2b.ps} } \end{figure}$	Figure 2: PICsIT minimum detectable flux for continuum (left panel) and narrow line (right panel) emission as a function of energy assuming only statistical effects, and the in-flight measured background. The dashed lines of the first two bins in the left panel indicate the worsening due to the effect of cosmic-ray induced tracks.
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$\begin{figure} \par\mbox{\includegraphics[scale=0.24,clip]{integral35_f3a.eps} \... ...f3c.eps} \includegraphics[scale=0.24,clip]{integral35_f3d.eps} } \end{figure}$	Figure 3: Crab significance images and profiles obtained from observations performed during revolution 43 with the standard ISDC/ISSW. Deconvolved images are shown for 4 energy bands: 203-252 keV, 252-329 keV, 329-455 keV, 455-655 keV.
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$\begin{figure} \par\includegraphics[scale=0.28,clip]{integral35_f4.eps} \end{figure}$	Figure 4: Cyg X-1 significance image and profile in the 252-329 keV band obtained from a 80 ks observation in revolution 11.
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