All Figures

$\begin{figure} \par\includegraphics[width=12cm,clip]{2763fig1.ps} \end{figure}$ Figure 1: VLT- Antu R-band image of the afterglow of GRB 000911 acquired on September 19, 2000. The field size is about 1 $\hbox {$.\mkern -4mu^\prime $ }2 \times 1 \hbox {$.\mkern -4mu^\prime $ }$ 2; North is at top, East is to the left. The OT is indicated by the tick marks, and several faint extended objects can be seen around it. The limiting magnitude of the image is $R \sim 25.5$ .
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{2763fig2.ps} \end{figure}$ Figure 2: Light curves of the afterglow of GRB 000911. Filled symbols represent our data, open symbols refer to the data reported in Lazzati et al. (2001) and Price et al. (2002). Different symbols correspond to different optical/NIR filters. The data are not corrected for Galactic extinction.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{2763fig3.ps} \end{figure}$ Figure 3: BVRIJH SFD of the host galaxy of GRB 000911 corrected for Galactic extinction (filled dots), superimposed onto one of the best-fit templates of Table 2 (a starburst-like galaxy plus intrinsic reddening) obtained applying the Hyperz code to the SFD data of the GRB 000911 host. The horizontal bars associated with the SFD data points indicate the FWHM of the photometric filters.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,bb=21 337 557 714,clip]{2763fig4.... ...\includegraphics[width=7cm,bb=21 134 270 311,clip]{2763fig4.ps}\par \end{figure}$ Figure 4: BVRIJ light curves of the GRB 000911 afterglow; in each panel, the time is computed since the GRB onset. The data are corrected for the Galactic extinction and then fitted with a power law with $\alpha = 1.48$ (oblique dashed line) plus a constant contribution due to the host galaxy (horizontal dashed line). The solid line represents the best-fit model. The last point in the I-band light curve represents the host galaxy value in this band, that is, the weighted average of the I-band measurements after December 2000 as described in the text and as reported in Table 3.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,bb=20 435 557 614,clip]{2763fig5.... ...mm} \includegraphics[width=7cm,bb=20 235 270 412,clip]{2763fig5.ps} \end{figure}$ Figure 5: Same as Fig. 4 for the RIJ light curves of the GRB 000911 afterglow, but with the addition of a SN1998bw at z = 1.06 (dot-dashed line; in the R-band panel this is not visible) brightened, with respect to the original one, by the factors reported in Table 3. The solid line represents the best-fit model. In these fits the SN explosion time was assumed to coincide with the GRB start time.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2763fig6.ps} \end{figure}$ Figure 6: SFDs of the afterglow of GRB 000911 at 1.44 (September 12.74, filled triangles), 5.03 (September 16.33, filled squares), 10.94 (September 22.24, empty squares), 16.90 (September 28.20, filled circles) and 25.00 (October 6.30, open triangles) days after GRB. The SFDs of September 12.74 and 16.33 are shifted up by 0.5 dex, while those of September 28.20 and October 6.30 are shifted down by 0.5 and 1.5 dex, respectively. The data are corrected for Galactic extinction and for the flux of the host galaxy.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{2763fig1.ps} \end{figure}$	Figure 1: VLT- Antu R-band image of the afterglow of GRB 000911 acquired on September 19, 2000. The field size is about 1 $\hbox {$.\mkern -4mu^\prime $ }2 \times 1 \hbox {$.\mkern -4mu^\prime $ }$ 2; North is at top, East is to the left. The OT is indicated by the tick marks, and several faint extended objects can be seen around it. The limiting magnitude of the image is $R \sim 25.5$ .
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$\begin{figure} \par\includegraphics[width=12cm,clip]{2763fig2.ps} \end{figure}$	Figure 2: Light curves of the afterglow of GRB 000911. Filled symbols represent our data, open symbols refer to the data reported in Lazzati et al. (2001) and Price et al. (2002). Different symbols correspond to different optical/NIR filters. The data are not corrected for Galactic extinction.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{2763fig3.ps} \end{figure}$	Figure 3: BVRIJH SFD of the host galaxy of GRB 000911 corrected for Galactic extinction (filled dots), superimposed onto one of the best-fit templates of Table 2 (a starburst-like galaxy plus intrinsic reddening) obtained applying the Hyperz code to the SFD data of the GRB 000911 host. The horizontal bars associated with the SFD data points indicate the FWHM of the photometric filters.
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