All Figures

$\begin{figure} \par\hspace*{2.5mm} \includegraphics[width=8cm,height=3.7cm,clip]... ...eps} \includegraphics[width=7.8cm,height=3.7cm,clip]{6391fig1b.eps} \end{figure}$ Figure 1: Upper panel: the Q, U plane of the stars in the field (circles) of XRF 060218 (square) imaged from CAHA on March 8.845 UT ( t-t₀ = 18.7 days). The size of each circle is proportional to the distance of the corresponding star to the center of the CCD. This is used to check that the instrumental polarization, if present, does not vary severely across the FoV. Lower panel: the satisfactory fit of the $S(\phi )$ function ( $\chi ^2/{\rm d.o.f.}=1.38$ ). As shown the XRF 060218/SN 2006aj is clearly polarized. An aperture radius = 1 FWHM was assumed.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{6391fig2.eps} \end{figure}$ Figure 2: The Stokes plane of 9 field stars and SN 2006aj on the combined AZT-8 image when the Galactic ISM correction is applied. The clouds of dots were created altering with a Montecarlo method the fluxes of the objects according to their photometric errors. The cloud representing SN 2006aj is shifted with respect to the origin defined by the field stars, assumed to be intrinsically unpolarized in average.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=7.4cm,clip]{6391fig3.eps} \end{figure}$ Figure 3: Our polarization results, once the the Galactic ISM correction was considered. Upper panel: as shown $\theta$ exhibited a rotation of $\sim$ $100^{\circ }$ at 5.6 < t-t₀ < 13.7 days. Middle panel: P shows a likely decay reaching a constant level at a $\sim$ $1.4\%$ level. Lower panel: the intrinsic $P_{\rm SN}$ evolution assuming that our last P detection is entirely originated by the host ISM. The dashed curves show the $\pm$ $1\sigma$ uncertainty region of the t^-2 decay, as seen in SN 2004dj.
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In the text