All Figures

$\begin{figure} \par\includegraphics[width=12cm,clip]{3950fi01.ps} \end{figure}$ Figure 1: X-ray spectra of the afterglows observed by BeppoSAX. Filled circles represent LECS data points and open circles represent MECS data points. Note that no LECS information was available for GRB 020410.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3950fi02.ps} \end{figure}$ Figure 2: The distribution of 1.6-10 keV fluxes in the BeppoSAX GRB afterglow sample. All fluxes are indicated 11 h after the burst. Upper limits have been set to 10^-13 for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{3950fi03.ps}\hspace*{4mm} \includegraphics[width=6.1cm,clip]{3950fi04.ps} \end{figure}$ Figure 3: Left: distribution of the spectral indexes of the afterglow of the BeppoSAX bursts. Right: distribution of the decay indexes of the afterglow of the BeppoSAX bursts.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3950fi05.ps} \end{figure}$ Figure 4: The 40-700 keV fluence distribution of the BeppoSAX GRB sample. Data are extracted from the literature.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{3950fi06.ps}\hspace*{4mm} \includegraphics[width=6.9cm,clip]{3950fi07.ps} \end{figure}$ Figure 5: Left: energy emitted during the prompt phase in the 40-700 keV band in the burst rest frame. The solid line represents the detection threshold of the GRBM discussed in the text. Right: energy emitted during the prompt phase in the 2-10 keV band in the burst rest frame. The solid line represents the detection threshold of the WFC discussed in the text.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3950fi08.ps} \end{figure}$ Figure 6: Distribution of the logarithmic ratios of the prompt $\gamma$ -ray fluence versus the X-ray afterglow flux for the BeppoSAX GRBsample.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3950fi09.ps} \end{figure}$ Figure 7: 1.6-10 keV afterglow luminosity vs. 40-700 keV energy of the prompt emission. The fit between these two quantities, discussed in the text, is also shown, together with its confidence interval (dot-dashed box). The correlation coefficient is r=0.74. The dotted lines represent Eq. (5) when $\epsilon _{\rm e}^{1.3}/\epsilon _{\gamma } = 10$ (upper line), 1 and 0.1 (middle lines), and 0.01 (lower line). The errors plotted here take the k-correction and measurement uncertainties into account.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3950fi10.ps} \end{figure}$ Figure 8: The closure relationships for all burst with constraints on both the spectral and temporal decay indexes. We indicate the closure relationships for the three cases (Jet expansion, Wind model, ISM model) in the three panels. Vertical lines indicate the theoretical expected values.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{3950fi11.ps} \end{figure}$ Figure 9: Afterglow luminosity of BeppoSAX GRBs with known redshift. Solid line: before correction for beaming. Dashed line: after correction for beaming.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{3950fi12.ps} \end{figure}$ Figure 10: Difference of the X-ray and optical decay indexes of BeppoSAX sample. Right line: $\delta _{\rm X}=\delta {\rm o}+0.25$ (as expected for an ISM environment). Left line: $\delta _{\rm X}=\delta {\rm o}-0.25$ (as expected for a wind environment). Uncertainties on the decay index values were not taken into account when building the histogram.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3950fi13.ps} \end{figure}$ Figure 11: Comparison of the $\gamma$ -ray fluences of dark (dotted line) and optically bright (dashed line) GRBs.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=6cm,angle=270]{3950fi14.ps}\hspa... ...pace{1cm} \includegraphics[width=6cm,angle=270]{3950fi19.ps} } \par \end{figure}$ Figure 12: X-ray lightcurves of the afterglows observed by beppoSAX in the 1.6-10 keV band.
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In the text

$\begin{figure}\par\mbox{\includegraphics[width=6cm,angle=270]{3950fi20.ps}\hspac... ...}\hspace{1cm} \includegraphics[width=6cm,angle=270]{3950fi25.ps} }\end{figure}$ Figure 12: continued.
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In the text

$\begin{figure}\par\mbox{\includegraphics[width=6cm,angle=270]{3950fi26.ps}\hspac... ...}\hspace{1cm} \includegraphics[width=6cm,angle=270]{3950fi31.ps} }\end{figure}$ Figure 12: continued.
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In the text

$\begin{figure}\par\mbox{\includegraphics[width=6cm,angle=270]{3950fi32.ps}\hspac... ...}\hspace{1cm} \includegraphics[width=6cm,angle=270]{3950fi37.ps} }\end{figure}$ Figure 12: continued.
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In the text

$\begin{figure}\par\mbox{\includegraphics[width=6cm,angle=270]{3950fi38.ps}\hspac... ...pace{1cm} \includegraphics[width=6cm,angle=270]{3950fi43.ps} } \par \end{figure}$ Figure 12: continued.
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In the text

$\begin{figure}\par\mbox{\includegraphics[width=6cm,angle=270]{3950fi44.ps}\hspac... ...}\hspace{1cm} \includegraphics[width=6cm,angle=270]{3950fi47.ps} }\end{figure}$ Figure 12: continued.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3950fi01.ps} \end{figure}$	Figure 1: X-ray spectra of the afterglows observed by BeppoSAX. Filled circles represent LECS data points and open circles represent MECS data points. Note that no LECS information was available for GRB 020410.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3950fi02.ps} \end{figure}$	Figure 2: The distribution of 1.6-10 keV fluxes in the BeppoSAX GRB afterglow sample. All fluxes are indicated 11 h after the burst. Upper limits have been set to 10^-13 for clarity.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{3950fi03.ps}\hspace*{4mm} \includegraphics[width=6.1cm,clip]{3950fi04.ps} \end{figure}$	Figure 3: Left: distribution of the spectral indexes of the afterglow of the BeppoSAX bursts. Right: distribution of the decay indexes of the afterglow of the BeppoSAX bursts.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3950fi05.ps} \end{figure}$	Figure 4: The 40-700 keV fluence distribution of the BeppoSAX GRB sample. Data are extracted from the literature.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{3950fi06.ps}\hspace*{4mm} \includegraphics[width=6.9cm,clip]{3950fi07.ps} \end{figure}$	Figure 5: Left: energy emitted during the prompt phase in the 40-700 keV band in the burst rest frame. The solid line represents the detection threshold of the GRBM discussed in the text. Right: energy emitted during the prompt phase in the 2-10 keV band in the burst rest frame. The solid line represents the detection threshold of the WFC discussed in the text.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3950fi08.ps} \end{figure}$	Figure 6: Distribution of the logarithmic ratios of the prompt $\gamma$ -ray fluence versus the X-ray afterglow flux for the BeppoSAX GRBsample.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3950fi10.ps} \end{figure}$	Figure 8: The closure relationships for all burst with constraints on both the spectral and temporal decay indexes. We indicate the closure relationships for the three cases (Jet expansion, Wind model, ISM model) in the three panels. Vertical lines indicate the theoretical expected values.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{3950fi11.ps} \end{figure}$	Figure 9: Afterglow luminosity of BeppoSAX GRBs with known redshift. Solid line: before correction for beaming. Dashed line: after correction for beaming.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{3950fi12.ps} \end{figure}$	Figure 10: Difference of the X-ray and optical decay indexes of BeppoSAX sample. Right line: $\delta _{\rm X}=\delta {\rm o}+0.25$ (as expected for an ISM environment). Left line: $\delta _{\rm X}=\delta {\rm o}-0.25$ (as expected for a wind environment). Uncertainties on the decay index values were not taken into account when building the histogram.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3950fi13.ps} \end{figure}$	Figure 11: Comparison of the $\gamma$ -ray fluences of dark (dotted line) and optically bright (dashed line) GRBs.
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$\begin{figure} \par\mbox{\includegraphics[width=6cm,angle=270]{3950fi14.ps}\hspa... ...pace{1cm} \includegraphics[width=6cm,angle=270]{3950fi19.ps} } \par \end{figure}$	Figure 12: X-ray lightcurves of the afterglows observed by beppoSAX in the 1.6-10 keV band.
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$\begin{figure}\par\mbox{\includegraphics[width=6cm,angle=270]{3950fi20.ps}\hspac... ...}\hspace{1cm} \includegraphics[width=6cm,angle=270]{3950fi25.ps} }\end{figure}$	Figure 12: continued.
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