All Figures

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{7619fig1.ps} \end{figure}$ Figure 1: The D-shaped BAT Field of View. Fully coded (100%), half-coded (50%) down to the 10% coded fraction contours are indicated.
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In the text

$\begin{figure} { \psfig{figure=7619fig2.ps,width=8cm,angle=-90} } \end{figure}$ Figure 2: Crab flux in the 10-100 keV energy band ( upper panel) and spectral photon index ( lower panel) as a function of the coded fraction, as estimated with the mask-weighting technique using celestial Crab coordinates. The horizontal dotted lines represent the best fit to the constant model (see Table 3 for details).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7619fig3.eps} \end{figure}$ Figure 3: Dispersion of Crab detection coordinates around the nominal source position (red cross). The coordinate dispersion is not perfectly centered on the Crab nominal position. Probably this is related to systematic image centroid shifts as a function of the position in the FOV (see BAT Digest pages), as well as to the distribution of the Crab detector coordinates in our dataset.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{7619fig4.ps} \end{figure}$ Figure 4: Crab flux in the 10-100 keV energy band ( upper panel) and spectral photon index ( lower panel) as a function of the coded fraction, as estimated with the mask-weighting technique using Crab detection coordinates. The horizontal dotted lines represent the best fit to the constant model (see Table 3 for details).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{7619fig5.ps} \end{figure}$ Figure 5: Flux difference using detection coordinates and nominal coordinates as a function of coordinate difference. Black squares represent the rows for which Crab was located at a coded fraction greater than 0.1, whereas red crosses are those for which the coded fraction was smaller than or equal to 0.1. The use of detection coordinates induces a slight source flux overestimate which can be quantified as $\sim$ 0.5%.
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In the text

$\begin{figure} { \psfig{figure=7619fig6.ps,width=16.5cm,angle=-90} }\end{figure}$ Figure 6: GRO J1655-40 complete 2005 outburst as seen from Swift/BAT and RXTE/HEXTE ( upper panel), RXTE/PCA ( central panel), and RXTE/ASM ( lower panel). In the upper panel, stars mark BAT and HEXTE points corresponding to averaged spectra. 3 $\sigma$ upper limits are also plotted, marked by arrows. Vertical dotted bars in the central and lower panels represent the time of the first detection of the outburst obtained with PCA and ASM respectively.
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In the text

$\begin{figure} \par\includegraphics[width=18cm]{7619fig7.eps} \end{figure}$ Figure 7: Left panels: zooms of three parts of the GRO J1655-40 outburst as seen by BAT (blue) and HEXTE (red) (symbols as in Fig. 6). The right panels represent the PCA count rate and hardness ratio as obtained from the (http://tahti.mit.edu/opensource/1655/) web site. The green box highlights the time span covered in the left panels.
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In the text

$\begin{figure} \par\psfig{figure=7619fig8.ps,width=9cm,angle=-90} \end{figure}$ Figure 8: Spectral photon index evolution of the GRO J1655-40 outburst as obtained by fitting a power law independently to BAT (blue) and HEXTE (red) spectra. Errors are given at a 1 $\sigma$ level. The star labeled BAT and HEXTE points correspond to averaged spectra.
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In the text

$\begin{figure} \par\psfig{figure=7619fig9.ps,width=9cm,angle=-90} \end{figure}$ Figure 9: Zoom of Fig. 8 for the central part of the outburst.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{7619fig1.ps} \end{figure}$	Figure 1: The D-shaped BAT Field of View. Fully coded (100%), half-coded (50%) down to the 10% coded fraction contours are indicated.
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$\begin{figure} { \psfig{figure=7619fig2.ps,width=8cm,angle=-90} } \end{figure}$	Figure 2: Crab flux in the 10-100 keV energy band ( upper panel) and spectral photon index ( lower panel) as a function of the coded fraction, as estimated with the mask-weighting technique using celestial Crab coordinates. The horizontal dotted lines represent the best fit to the constant model (see Table 3 for details).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{7619fig3.eps} \end{figure}$	Figure 3: Dispersion of Crab detection coordinates around the nominal source position (red cross). The coordinate dispersion is not perfectly centered on the Crab nominal position. Probably this is related to systematic image centroid shifts as a function of the position in the FOV (see BAT Digest pages), as well as to the distribution of the Crab detector coordinates in our dataset.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{7619fig4.ps} \end{figure}$	Figure 4: Crab flux in the 10-100 keV energy band ( upper panel) and spectral photon index ( lower panel) as a function of the coded fraction, as estimated with the mask-weighting technique using Crab detection coordinates. The horizontal dotted lines represent the best fit to the constant model (see Table 3 for details).
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$\begin{figure} \par\includegraphics[width=18cm]{7619fig7.eps} \end{figure}$	Figure 7: Left panels: zooms of three parts of the GRO J1655-40 outburst as seen by BAT (blue) and HEXTE (red) (symbols as in Fig. 6). The right panels represent the PCA count rate and hardness ratio as obtained from the (http://tahti.mit.edu/opensource/1655/) web site. The green box highlights the time span covered in the left panels.
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$\begin{figure} \par\psfig{figure=7619fig8.ps,width=9cm,angle=-90} \end{figure}$	Figure 8: Spectral photon index evolution of the GRO J1655-40 outburst as obtained by fitting a power law independently to BAT (blue) and HEXTE (red) spectra. Errors are given at a 1 $\sigma$ level. The star labeled BAT and HEXTE points correspond to averaged spectra.
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$\begin{figure} \par\psfig{figure=7619fig9.ps,width=9cm,angle=-90} \end{figure}$	Figure 9: Zoom of Fig. 8 for the central part of the outburst.
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