All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1267fig1.ps} \end{figure}$ Figure 1: Light curves of GRB 040106 beginning at 17:55 UTC extracted from ( top to bottom) IBIS/ISGRI data in the range 15-40 keV, IBIS/ISGRI data in the range 40-200 keV, SPI scientific housekeeping data in the range 20 keV-8 MeV and ( bottom panel) the hardness ratio evolution derived from IBIS/ISGRI count rates.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1267fig2.ps} \end{figure}$ Figure 2: Background subtracted EPIC light curve of the X-ray afterglow of GRB 040106 in the 0.4-10 keV energy band. The dashed line shows the best-fit power-law decay $\delta$ = 1.46.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1267fig3.ps} \end{figure}$ Figure 3: EPIC spectrum of the GRB 040106 afterglow and its best-fit absorbed power-law model. The upper data points refer to PN while the lower ones to MOS1 and MOS2. The residuals are in units of standard deviations.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.35cm,clip]{1267fig4.ps} \end{figure}$ Figure 4: Extrapolated 2-10 keV fluxes from SPI (circles) and IBIS (squares) for each of the two pulses. The solid line is the extrapolation of the X-ray data while the dashed lines represent the range of decay slopes based on the power-law decay of the 2nd pulse.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1267fig1.ps} \end{figure}$	Figure 1: Light curves of GRB 040106 beginning at 17:55 UTC extracted from ( top to bottom) IBIS/ISGRI data in the range 15-40 keV, IBIS/ISGRI data in the range 40-200 keV, SPI scientific housekeeping data in the range 20 keV-8 MeV and ( bottom panel) the hardness ratio evolution derived from IBIS/ISGRI count rates.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1267fig2.ps} \end{figure}$	Figure 2: Background subtracted EPIC light curve of the X-ray afterglow of GRB 040106 in the 0.4-10 keV energy band. The dashed line shows the best-fit power-law decay $\delta$ = 1.46.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1267fig3.ps} \end{figure}$	Figure 3: EPIC spectrum of the GRB 040106 afterglow and its best-fit absorbed power-law model. The upper data points refer to PN while the lower ones to MOS1 and MOS2. The residuals are in units of standard deviations.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.35cm,clip]{1267fig4.ps} \end{figure}$	Figure 4: Extrapolated 2-10 keV fluxes from SPI (circles) and IBIS (squares) for each of the two pulses. The solid line is the extrapolation of the X-ray data while the dashed lines represent the range of decay slopes based on the power-law decay of the 2nd pulse.
Open with DEXTER