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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fc184_f1} \end{figure}$ Figure 1: A plot of the Stokes vectors ( $\ensuremath {Q}$ , $\ensuremath {U}$ ) and their error bars (1- $\sigma$ of the afterglow at different epochs, and of the field stars as determined by the FORS 1 observation. The afterglow is annotated with the time after the burst in days. The ALFOSC measurements are denoted with an asterisk and the FORS 1 measurement with a square. We have also included data from the Covino et al. (2002b,c) (denoted with a triangle) and from Wang et al. (2003) (diamond). The field stars are plotted without symbols. The dashed ellipse encloses the surface which contains 68% of the field stars, according to their measured spread. The weighted mean ( $\ensuremath {Q}$ , $\ensuremath {U}$ ) value of the field stars is represented by the thick cross, where the size of the cross indicates the error in the mean. We have used the spread in the field stars as the error in the ISM induced polarization, rather than the error in the weighted mean.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fc184_f2.eps} \end{figure}$ Figure 2: A plot of the degree of linear polarization P and the position angle $\theta$ as function of time. ALFOSC measurements are indicated with an asterisk, the FORS 1 measurement with a square. We have included the data from Covino et al. (2002b,c) and from Wang et al. (2003, diamond). The dashed lines give the $\pm$ 1- $\sigma$ ranges for the ISM polarization.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fc184_f2.eps} \end{figure}$	Figure 2: A plot of the degree of linear polarization P and the position angle $\theta$ as function of time. ALFOSC measurements are indicated with an asterisk, the FORS 1 measurement with a square. We have included the data from Covino et al. (2002b,c) and from Wang et al. (2003, diamond). The dashed lines give the $\pm$ 1- $\sigma$ ranges for the ISM polarization.
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