All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Ej101_fig1_bw.eps} \end{figure}$ Figure 1: The field of GRB 020813 ( $\sim$ $1.5\hbox {$^\prime $ }\times 1.5\hbox {$^\prime $ }$ ), as imaged by TNG-DOLORES on Aug. 15 UT. The afterglow is marked by an arrow. This is a composite image from B, V, and R filters. North is up, East is left.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aaej101f2.eps} \end{figure}$ Figure 2: Optical and NIR light curves of GRB 020813 afterglow, with our best fit according to Eq. (1) (dashed lines); refer to Table 1 for fit parameters, and to the web page for the numerical values. For the first night (t<5 h), error bars are smaller than symbols and are not plotted. The thick solid line shows the (arbitrarily normalized) X-ray decay.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Ej101_fig3_bw.ps} \end{figure}$ Figure 3: a) Photometric spectra of GRB 028013 afterglow at various times (see Table 2), together with the best fit (dotted lines). Data are corrected for reddening in the Galaxy but not in the host. Error bars are smaller than the symbols and are not plotted. b) TNG spectrum on Aug. 15.04 UT; open points and dotted line are corrected only for Galactic reddening, while filled points and dot-dashed line are corrected also for reddening in the host (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aaej101f4.eps} \end{figure}$ Figure 4: Radio to X-ray spectral energy distribution of the afterglow of GRB 020813, 30 h after the trigger. Optical ( BVRI bands) and X-ray data have been computed at the epoch of the radio detection by interpolating between different spectra and using the appropriate decay law. Open symbols are corrected only for Galactic extinction, while the additional host component has been taken into account for filled symbols. Radio detection together with the millimeter upper bounds limit the spectral slope ( $F_\nu \propto \nu ^{-\alpha }$ ) to be $\alpha \ge -1/3$ at GHz frequencies (in particular a self-absorbed spectrum is ruled out). In the region between the millimeter and optical bands, the drawing is only indicative.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Ej101_fig1_bw.eps} \end{figure}$	Figure 1: The field of GRB 020813 ( $\sim$ $1.5\hbox {$^\prime $ }\times 1.5\hbox {$^\prime $ }$ ), as imaged by TNG-DOLORES on Aug. 15 UT. The afterglow is marked by an arrow. This is a composite image from B, V, and R filters. North is up, East is left.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aaej101f2.eps} \end{figure}$	Figure 2: Optical and NIR light curves of GRB 020813 afterglow, with our best fit according to Eq. (1) (dashed lines); refer to Table 1 for fit parameters, and to the web page for the numerical values. For the first night (t<5 h), error bars are smaller than symbols and are not plotted. The thick solid line shows the (arbitrarily normalized) X-ray decay.
Open with DEXTER