All Figures

$\begin{figure} \par\includegraphics[width=7.8cm]{3903fig1.ps} \end{figure}$ Figure 1: Light curves of the bursts with a good constraint on both the spectral and temporal indexes. We have indicated in blue the XMM-Newton bursts, in black the Chandra Grating bursts and in red the Chandra Imaging bursts (see electronic version for color).
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In the text

$\begin{figure} \par {\includegraphics[width=8cm]{3903fig2.ps} } % \end{figure}$ Figure 2: Cumulative distribution of flux of the afterglows observed by XMM-Newton (dashed line) and Swift-XRT (continuous line) 12 h after the burst.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{3903fig3.ps} } \end{figure}$ Figure 3: The closure relationships for all bursts with constraints on both the spectral and temporal decay indexes. We indicate the closures for the three cases (Jet effects, Wind model, ISM model) in the three panels. Vertical lines indicate the theoretical expected values. Afterglows observed by Chandra are located at the top (in red for Chandra Imaging and in black for Chandra Grating data), while those observed by XMM-Newton are located at the bottom (in blue, see electronic version for colors).
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{3903fig4.ps} \end{figure}$ Figure 4: Composite light curve of an X-ray afterglow. XMM-Newton bursts are in blue, Chandra Grating bursts in black, Chandra-Imaging bursts in red. Points relative to the same afterglow are connected by a solid line. The two dashed purple lines represent the mean decay observed from XMM-Newton and Chandra Imaging bursts.
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In the text

$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{3903fig5.ps} } % \end{figure}$ Figure 5: Distributions of the isotropic luminosity for all BeppoSAX, XMM-Newton or Chandra bursts with good constraints on the spectral and temporal decay index and known redshift (top panel), for a sub-sample of bursts with known beaming angle (middle panel), and distribution of the beaming corrected luminosity of this sub-panel (bottom panel) using the method of Berger et al. (2003). All luminosities were calculated at 11 h after the burst (in the burst rest frame), using the observed values of spectral index, temporal decay, redshift and beaming angle. The low luminosity outlier in the top panel is GRB 031203, not plotted in the two other panels.
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm]{3903fig6.ps} \end{figure}$ Figure 6: X-ray absorption versus redshift. We indicate in this figure all detected absorptions or the corresponding upper limits for all bursts bright enough for a spectral study. The redshift was assumed to be one when not available.
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In the text

$\begin{figure} \par {\includegraphics[width=7cm,clip]{3903fig7.ps} } \end{figure}$ Figure 7: Optical versus X-ray fluxes of GRB afterglows 11 h after the burst. Squares and open circles represent XMM-Newton and Beppo-SAX data (extracted from De Pasquale et al. 2003) respectively. Lines indicate the best fit relationships (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm]{3903fig1.ps} \end{figure}$	Figure 1: Light curves of the bursts with a good constraint on both the spectral and temporal indexes. We have indicated in blue the XMM-Newton bursts, in black the Chandra Grating bursts and in red the Chandra Imaging bursts (see electronic version for color).
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$\begin{figure} \par {\includegraphics[width=8cm]{3903fig2.ps} } % \end{figure}$	Figure 2: Cumulative distribution of flux of the afterglows observed by XMM-Newton (dashed line) and Swift-XRT (continuous line) 12 h after the burst.
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$\begin{figure} \par\includegraphics[width=8cm]{3903fig4.ps} \end{figure}$	Figure 4: Composite light curve of an X-ray afterglow. XMM-Newton bursts are in blue, Chandra Grating bursts in black, Chandra-Imaging bursts in red. Points relative to the same afterglow are connected by a solid line. The two dashed purple lines represent the mean decay observed from XMM-Newton and Chandra Imaging bursts.
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$\begin{figure} \par\includegraphics[width=6.4cm]{3903fig6.ps} \end{figure}$	Figure 6: X-ray absorption versus redshift. We indicate in this figure all detected absorptions or the corresponding upper limits for all bursts bright enough for a spectral study. The redshift was assumed to be one when not available.
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$\begin{figure} \par {\includegraphics[width=7cm,clip]{3903fig7.ps} } \end{figure}$	Figure 7: Optical versus X-ray fluxes of GRB afterglows 11 h after the burst. Squares and open circles represent XMM-Newton and Beppo-SAX data (extracted from De Pasquale et al. 2003) respectively. Lines indicate the best fit relationships (see text for details).
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