All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{INTEGRAL60_f1.eps} \end{figure}$ Figure 1: Evolution of the number of disabled ISGRI pixels (black solid line), and number of pixels which efficiency is higher (dashed line) and less (dotted line) than 70%, from revolution 35 (starting on 01/21/03) to 80 (ending on 06/12/03). The introduction of the new pixel thresholding algorithm during revolution 54 removed progressively most of the bad pixels.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{INTEGRAL60_f2.eps} \end{figure}$ Figure 2: ISGRI in-flight calibration data spectrum, after thermal and charge loss corrections. Note the large line at around 25 keV and the four lead and tungsten fluorescence lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{INTEGRAL60_f3.eps} \end{figure}$ Figure 3: Effective temperature map on the camera: relative temperature variation between the thermal sensor number 3 and the temperature deduced from the pixel gains. A module per module structure is clearly visible, as well as a thermal gradient along the z-axis. Numbers indicates MDU thermal sensors positions in the camera.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{INTEGRAL60_f4.eps} \end{figure}$ Figure 4: Variation of energy resolution ( FWHM) with rise time at 59.3 keV and 511 keV. The strong degradation with rise times comes from the remaining miscalibations of rise time gains and offset. Note that the 59.3 keV resolution is not given above 2.6 ${\rm\mu s}$ because the tungsten $K\alpha$ line is mixed up with $K\beta$ and lead fluorescence lines.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{INTEGRAL60_f5.eps} \end{figure}$ Figure 5: In flight biparametric diagram obtained with calibration unit data. Superimposed is the charge correction dependency from the LUT2 for the 59.3 keV and 511 keV lines. The background displays an unexpected high rise time structure covering the whole amplitude range. This strongly limits the sensitivity at high rise times, therefore an on-board upper limit selection has been implemented. A second unexpected structure can also be seen with pulse height increasing with rise time. The origin of these structures is unclear.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{INTEGRAL60_f6.eps} \end{figure}$ Figure 6: Effect of noise substraction on mosaic images in various energy bands (20-40 keV, 40-100 keV, 100-200 keV, 200-400 keV). First column show the background model shadowgram, second column the mosaic of significance obtained without background substraction and third column the same mosaic after substraction. Significance values range from $-5\sigma$ (black) to $5\sigma$ (white). Strong background features in particular in intermediate energy bands are clearly removed. Some residual structure is still visible and is currently under investigation.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{INTEGRAL60_f1.eps} \end{figure}$	Figure 1: Evolution of the number of disabled ISGRI pixels (black solid line), and number of pixels which efficiency is higher (dashed line) and less (dotted line) than 70%, from revolution 35 (starting on 01/21/03) to 80 (ending on 06/12/03). The introduction of the new pixel thresholding algorithm during revolution 54 removed progressively most of the bad pixels.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{INTEGRAL60_f2.eps} \end{figure}$	Figure 2: ISGRI in-flight calibration data spectrum, after thermal and charge loss corrections. Note the large line at around 25 keV and the four lead and tungsten fluorescence lines.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{INTEGRAL60_f3.eps} \end{figure}$	Figure 3: Effective temperature map on the camera: relative temperature variation between the thermal sensor number 3 and the temperature deduced from the pixel gains. A module per module structure is clearly visible, as well as a thermal gradient along the z-axis. Numbers indicates MDU thermal sensors positions in the camera.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{INTEGRAL60_f4.eps} \end{figure}$	Figure 4: Variation of energy resolution ( FWHM) with rise time at 59.3 keV and 511 keV. The strong degradation with rise times comes from the remaining miscalibations of rise time gains and offset. Note that the 59.3 keV resolution is not given above 2.6 ${\rm\mu s}$ because the tungsten $K\alpha$ line is mixed up with $K\beta$ and lead fluorescence lines.
Open with DEXTER