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Figure 1: Dereddened flux of Sgr A* ( top) and of the two comparison stars W6 and S7 ( second from top) at the different polarization angles. The comparison stars are located within < of Sgr A*. Due to the presence of two stellar sources at the position of Sgr A* (see Fig. 1 in Eisenhauer et al. 2005), its lightcurve stays at a constant level of about 5 mJy after the flare. The light curves of the channels have been calibrated to an overall polarization of at an angle east of north (Eckart et al. 1995; Ott et al. 1999). Also, the curves are shifted to the total flux of the sources, i.e. the flux per channel is only half of the flux shown in the plots. The inferred polarization angle and the degree of linear polarization of Sgr A* can be seen in the bottom panels.

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In the text

	Figure 2: Periodogram of the light curves of Sgr A* for all four observed polarization angles. The periodogram has been oversampled by a factor of 2.
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In the text

	Figure 3: The best fit solution (in red) for the constant E-vector case. Shown is the flux ( top), the polarization angle ( middle), and the degree of linear polarization ( bottom). The parameters of the model are , . The spot is orbiting at a radius r=4 GM/c2. The disk/ring and the spot both have an intrinsic polarization degree of 17%.
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In the text

Figure 4: Confidence contours for the constant E-Vector case ( top) and the azimuthal magnetic field ( bottom). The red (green) lines are chosen such that the projection onto one of the parameter axes gives the 1 (3) limit for this parameter. The blue dashed lines indicate the 3 contour for the 2005 data, analyzed by Meyer et al. (2006). The -minimum for the 2006 data is marked by the big cross. The -minimum of the 2005 epoch lies at , ( top) and , ( bottom). Our analysis is limited to , see Meyer et al. (2006).

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In the text