$\begin{figure} \par\includegraphics[width=7.2cm,clip]{4811fig1.eps} \end{figure}$ Figure 1: Lightcurve of GRB 030406 seen by the INTEGRAL sub-systems: SPI-ACS, IBIS/ISGRI, IBIS Compton and IBIS/PICsIT. The gray areas: precursor, peak and tail correspond to the time regions chosen for spectral analysis. Time = 0 corresponds to the SPI-ACS trigger time at UTC 2003-04-06, 22:42:03.23.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{4811fig2.eps}\end{figure}$ Figure 2: All-sky Compton map taken during the second peak of the GRB 030406. The inset shows the dashed area around the GRB 030406 centered on the IPN position.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4811fig3.eps} \end{figure}$ Figure 3: The normalized cumulative distribution of the offset of best fit localizations of simulated bursts obtained in the Monte Carlo simulation: 68% of the events are localized within $\sim$ $4^\circ$ of the actual position.
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In the text

$\begin{figure} \mbox{\hspace*{2.5cm}{\em precursor}\hspace*{5cm}{\em peak}\hspac... ...4811fig9.eps}\hspace{0.7cm}\includegraphics[angle=0]{4811fig7.eps}} \end{figure}$ Figure 4: GRB 030406 spectrum fits to the combined ISGRI and Compton mode data. Upper panels show count spectra, while lower corresponding $\nu {\rm F}_\nu$ spectra. Broken power law model was fitted in each case: to the precursor data ( left), to the peak part data ( center) and to the tail ( right). See text for details.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4811fig0.eps} \end{figure}$ Figure 5: Confidence limits on $E_{\rm cutoff}$ : the solid line represents the $\chi ^2$ as a function of $E_{\rm cutoff}$ using the model of Eq. (1). We present the $\chi ^2$ values corresponding to the 90% and 99% confidence levels.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{4811fig1.eps} \end{figure}$	Figure 1: Lightcurve of GRB 030406 seen by the INTEGRAL sub-systems: SPI-ACS, IBIS/ISGRI, IBIS Compton and IBIS/PICsIT. The gray areas: precursor, peak and tail correspond to the time regions chosen for spectral analysis. Time = 0 corresponds to the SPI-ACS trigger time at UTC 2003-04-06, 22:42:03.23.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{4811fig2.eps}\end{figure}$	Figure 2: All-sky Compton map taken during the second peak of the GRB 030406. The inset shows the dashed area around the GRB 030406 centered on the IPN position.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4811fig3.eps} \end{figure}$	Figure 3: The normalized cumulative distribution of the offset of best fit localizations of simulated bursts obtained in the Monte Carlo simulation: 68% of the events are localized within $\sim$ $4^\circ$ of the actual position.
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$\begin{figure} \mbox{\hspace{2.5cm}{\em precursor}\hspace{5cm}{\em peak}\hspac... ...4811fig9.eps}\hspace{0.7cm}\includegraphics[angle=0]{4811fig7.eps}} \end{figure}$	Figure 4: GRB 030406 spectrum fits to the combined ISGRI and Compton mode data. Upper panels show count spectra, while lower corresponding $\nu {\rm F}_\nu$ spectra. Broken power law model was fitted in each case: to the precursor data ( left), to the peak part data ( center) and to the tail ( right). See text for details.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4811fig0.eps} \end{figure}$	Figure 5: Confidence limits on $E_{\rm cutoff}$ : the solid line represents the $\chi ^2$ as a function of $E_{\rm cutoff}$ using the model of Eq. (1). We present the $\chi ^2$ values corresponding to the 90% and 99% confidence levels.
Open with DEXTER