All Figures

$\begin{figure} \par\resizebox{7cm}{!}{\includegraphics[angle=270]{5925Flux.eps}}\par\resizebox{7cm}{!}{\includegraphics[angle=270]{5925Peri.eps}} \par\end{figure}$ Figure 1: Sgr A* NIR flare from 16 June 2003. Upper panel: light curve of Sgr A* in black. A polynome fit to the overall flare and the residuals after subtracting this fit are shown in red. The light curve of a constant star, S1, is shown in green. Lower panel: periodogram of the Sgr A* flare after subtraction of the overall flare, i.e. corresponding to the lower, red curve in the upper panel. The straight red line shows a de-biased power law fit to the data points when considering all frequencies greater than $2\times 10^{-3}$ Hz. The dashed lines give the 1-, 2-, 3- and $5\sigma$ confidence bands derived with the method of Vaughan (2005).
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In the text

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics{5925Cart.eps}} \end{figure}$ Figure 2: Sketch of the Newtonian behaviour of the E-vector (red) for the two magnetic field configurations. The black circle represents the MBH, the ellipse within the equatorial plane indicates a projected Keplerian orbit of a hot spot in the local comoving frame. Left: the case where the E-vector is always constant. Right: the case of an azimuthal magnetic field (like the ellipse) where the E-vector of the emitted synchrotron radiation rotates.
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In the text

$\begin{figure} \par\resizebox{7.5cm}{!}{\includegraphics[angle=270]{5925fit1-New... ...\par\resizebox{7.5cm}{!}{\includegraphics[angle=270]{5925fit3.eps}} \end{figure}$ Figure 3: The best fit solution (in red) for a constant E-vector. Shown is the flux ( top), polarization angle ( middle), and polarization degree ( bottom). The parameters of the model are $i = 70\hbox {$^\circ $ }$ , $a_\star \approx 1$ , a location of the projection of the disk on the sky of $100\hbox {$^\circ $ }$ and a polarization degree of the disk (spot) of $4\%$ ( $60\%$ ). The spot is orbiting at a radius $r=4.4 r_{\rm g}$ .
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In the text

$\begin{figure} \par\resizebox{7.5cm}{!}{\includegraphics[angle=270]{5925fit4.eps... ...\par\resizebox{7.5cm}{!}{\includegraphics[angle=270]{5925fit6.eps}} \end{figure}$ Figure 4: The best fit solution (in red) for a global azimuthal magnetic field. Shown is the flux ( top), polarization angle ( middle), and polarization degree ( bottom). The parameters of the model are ${i}~=~70\hbox{$^\circ$ }$ , $a_\star \approx 0.5$ , a location of the projection of the disk on the sky of $0\hbox {$^\circ $ }$ and a polarization degree of the disk (spot) of $9\%$ ( $60\%$ ). The spot is orbiting at a radius $r=4.5 r_{\rm g}$ .
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In the text

$\begin{figure} \par\resizebox{7cm}{!}{\includegraphics[angle=270]{5925Con1.eps}}\par\resizebox{7cm}{!}{\includegraphics[angle=270]{5925Con2.eps}} \end{figure}$ Figure 5: The confidence contours for the constant E-vector ( top) and the azimuthal magnetic field case ( bottom). The red (green) line is chosen such that the projection onto one of the parameter axes gives the $1\sigma$ ( $3\sigma$ ) limit for this parameter. The respective $\chi ^2$ -minimum is marked by the big cross. Note the different scales on the abscissae.
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In the text

$\begin{figure} \par\resizebox{7cm}{!}{\includegraphics[angle=270]{5925Con1.eps}}\par\resizebox{7cm}{!}{\includegraphics[angle=270]{5925Con2.eps}} \end{figure}$	Figure 5: The confidence contours for the constant E-vector ( top) and the azimuthal magnetic field case ( bottom). The red (green) line is chosen such that the projection onto one of the parameter axes gives the $1\sigma$ ( $3\sigma$ ) limit for this parameter. The respective $\chi ^2$ -minimum is marked by the big cross. Note the different scales on the abscissae.
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