All Figures

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig1.ps} \end{figure}$ Figure 1: Synchrotron (dot-dashed lines) and SSC (dashed lines) prompt emission spectra for a burst at redshift z=1. The burst prompt emission luminosity is L₅₂=1 and its variability is $t_{\rm v}=1~\rm ms$ . We fix the fraction of fireball energy going into relativistic electrons and magnetic field to $\epsilon _{\rm e}=0.45$ and $\epsilon _B=0.1$ respectively, and fix p=2.5. We display the predicted spectra for three different values of the fireball Lorentz factor $\Gamma$ : 200 (purple), 350 (blue) and 650 (red). The solid lines and the dot-dot-dot-dashed lines represent AGILE and GLAST sensitivity for an integration time of 10 s (in grey) and 50 s (in black). The solid vertical lines refer to the Swift XRT (red) and BAT (black) energy ranges.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig2.ps} \end{figure}$ Figure 2: Synchrotron (dot-dashed lines) and SSC (dashed lines) prompt emission spectra for a burst at redshift z=1.0. The fireball Lorentz factor is fixed to $\Gamma =600$ , and the other parameters are the same as in Fig. 1. We display the predicted spectra for three different values of the burst temporal variability $t_{\rm v}$ : 0.1 ms (red), 1.0 ms (blue) and 10 ms (purple). The solid lines and the dot-dot-dot-dashed lines represent AGILE and GLAST sensitivity for an integration time of 10 s (in grey) and 50 s (in black). The solid vertical lines refer to the Swift XRT (red) and BAT (black) energy ranges.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig3.ps} \end{figure}$ Figure 3: Distribution of peak times of the total (with and without redshift) flare sample of Chincarini et al. (2007b) (in grey), and of the sub-sample of flares with known redshift (in purple) reported in Table 2.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig4.ps} \end{figure}$ Figure 4: Distribution of the flare duration of the complete sample of flare from Chincarini et al. (2007b) (in grey), and of the sub-sample of flares with known redshift reported in Table 2 (in purple).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig5.ps} \end{figure}$ Figure 5: Redshift distribution of the flares of our sample.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig6.ps} \end{figure}$ Figure 6: Luminosity distribution of the flares of our sample.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig7.ps} \end{figure}$ Figure 7: Synchrotron (dot-dashed lines) and SSC (dashed lines) spectra for an X-ray flare with luminosity $L=2 \times 10^{49}~\rm erg~s^{-1}$ and temporal variability $t_{\rm v}=100$ ms at redshift z=1 as a function of the fireball Lorentz factor $\Gamma$ . Other model parameters are the same as in Fig. 1. We display the predicted spectra for $\Gamma =100$ (red) and $\Gamma =300$ (blue). The solid and dot-dot-dot-dashed lines represent AGILE and GLAST sensitivity for an integration time of 100 s (in grey) and 500 s (in black). The solid vertical lines refer to the Swift XRT (red) and BAT (black) energy ranges.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig8.ps} \end{figure}$ Figure 8: Synchrotron (dot-dashed lines) and SSC (dashed lines) spectra for an X-ray flare with luminosity $L= 10^{50}~\rm erg~s^{-1}$ and temporal variability $t_{\rm v}=100$ ms at redshift z=1 as a function of the fireball Lorentz factor $\Gamma$ . The other model parameters are the same of Fig. 1. We display the predicted spectra for $\Gamma =100$ (red) and $\Gamma =300$ (blue). The solid and dot-dot-dot-dashed lines represent AGILE and GLAST sensitivity for an integration time of 100 s (in grey) and 500 s (in black). The solid vertical lines refer to the Swift XRT (red) and BAT (black) energy ranges.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig9.ps} \end{figure}$ Figure 9: Synchrotron (dot-dashed lines) and SSC (dashed) spectra for an X-ray flare with luminosity $L=2 \times 10^{49}~\rm erg~s^{-1}$ and temporal variability $t_{\rm v}=100$ ms at redshift z=1 as a function of $\epsilon _B$ . The fireball Lorentz factor is fixed to $\Gamma =100$ , and other model parameters are the same as in Fig. 1. We display the predicted spectra for $\epsilon _B=0.1$ (red), $\epsilon _B=0.01$ (blue) and $\epsilon _B=0.001$ (purple). The solid and dot-dot-dot-dashed lines represent the AGILE and GLAST sensitivities for an integration time of 100 s (in grey) and 500 s (in black). The solid vertical lines refer to the Swift XRT (red) and BAT (black) energy ranges.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fi10.ps} \end{figure}$ Figure 10: Synchrotron (dot-dashed lines) and SSC (dashed) spectra for an X-ray flare with luminosity $L=2 \times 10^{49}~\rm erg~s^{-1}$ as a function of the temporal variability $t_{\rm v}$ at redshift z=1. The fireball Lorentz factor is fixed to $\Gamma =100$ and other model parameters are the same as in Fig. 1. We display the predicted spectra for $t_{\rm v}=10$ ms (red), $t_{\rm v}=100$ ms (blue) and $t_{\rm v}=1$ s (purple). The solid and dot-dot-dot-dashed lines represent the AGILE and GLAST sensitivities for an integration time of 100 s (in grey) and 500 s (in black). The solid vertical lines refer to the Swift XRT (red) and BAT (black) energy ranges.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fi11.ps} \end{figure}$ Figure 11: Synchrotron (dot-dashed lines) and SSC (dashed lines) spectra for a typical X-ray flare with luminosity $L=2 \times 10^{49}~\rm erg~s^{-1}$ and temporal variability $t_{\rm v}=40~$ s at redshift z=1 as a function of the fireball Lorentz factor $\Gamma$ . Other model parameters are the same as in Fig. 1. We display the predicted spectra for $\Gamma =10$ (red), $\Gamma =25$ (blue) and $\Gamma =50$ (purple). The solid and dot-dot-dot-dashed lines represent AGILE and GLAST sensitivity for an integration time of 100 s (in grey) and 500 s (in black). The solid vertical lines refer to the Swift XRT (red) and BAT (black) energy ranges.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig3.ps} \end{figure}$	Figure 3: Distribution of peak times of the total (with and without redshift) flare sample of Chincarini et al. (2007b) (in grey), and of the sub-sample of flares with known redshift (in purple) reported in Table 2.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig4.ps} \end{figure}$	Figure 4: Distribution of the flare duration of the complete sample of flare from Chincarini et al. (2007b) (in grey), and of the sub-sample of flares with known redshift reported in Table 2 (in purple).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig5.ps} \end{figure}$	Figure 5: Redshift distribution of the flares of our sample.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.0cm,height=9.16cm,angle=90]{8518fig6.ps} \end{figure}$	Figure 6: Luminosity distribution of the flares of our sample.
Open with DEXTER