All Figures

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2935fig1.eps} \end{figure}$ Figure 1: Beam geometry of the VTT (sketch not to scale). The coelostat consists of two flat aluminum-coated mirrors (C1 and C2), which feed the light beam into the telescope. M3 is the imaging mirror (f=46 m). M4 folds the light down to the laboratories. E1 and E2 are the entrance and exit windows of the evacuated tube. The Instrument Calibration Unit (ICU) is located below the exit window.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2935fig2.ps} \end{figure}$ Figure 2: Response of the telescope proper to linearly polarized light at 630 nm, as the telescope calibration unit was rotated by 180 $^\circ$ in steps of 10 $^\circ$ . From top to bottom the four Stokes parameters are shown for 5 different times during the day.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2935fig3.ps} \end{figure}$ Figure 3: For three wavelengths (518/630/777 nm), the Mueller matrix entries $\cal M$ (1,1), $\cal M$ (1,2), $\cal M$ (1,3), $\cal M$ (2,3), and $\cal M$ (3,3) ( top to bottom) of a mirror sample were measured as function of the angle of incidence, i. The measurements could be reproduced using the refractive indices given in the uppermost panel.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2935fig4.ps} \end{figure}$ Figure 4: The daily variation of the continuum polarization at 630 nm induced by the telescope on July 28, 2003 with C1 at $\gamma =0^{\circ }$ . The solid curve corresponds to the prediction of the telescope model with n=1.41 and k=7.6.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2935fig5.ps} \end{figure}$ Figure 5: Same as Fig. 4 for an observation of a sunspot on August 9, 2003, from UT 9:30 to 10:30.
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In the text

$\begin{figure} \par\includegraphics[width=4cm,clip]{2935fig6.eps} \end{figure}$ Figure A.1: Sketch of reflection on a flat mirror. The incoming ray is described in the right-handed orthogonal coordinate system given by $\{\hat{x}, \hat{y}, \hat{z}\}$ , the reflected beam in the primed one. $\hat{x}$ and $\hat{x}^\prime$ lie in the incidence-reflection plane, while $\hat{y}$ and $\hat{y}^\prime$ are parallel to the mirror surface. i denotes the angle of incidence.

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2935fig7.eps} \end{figure}$ Figure C.1: The coelostat in the equatorial and horizontal coordinate system. The origin is placed in the center of C1.

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2935fig8.ps} \end{figure}$ Figure D.1: The change of the orientation angle of the linear polarization, $\beta _{\rm in}-\beta _{\rm out}$ , during the day (solid line). The dash-dotted line is the prediction of Eq. (D.1) for the rotation angle. The increase in the rotation angle is caused by the changing declination of the Sun, while the differences are the result of numerical inaccuracies.

In the text

$\begin{figure} \par\includegraphics[width=16.3cm,clip]{2935fig9.ps} \end{figure}$ Figure E.1: Daily variation of the 16 entries of the telescope Mueller matrix, $\cal T$ , for two dates: March 21 (black, $\delta _\odot \sim 0^\circ$ , $\gamma = \pm 50^\circ$ ) and July 28 (grey, $\delta _\odot \sim 20^\circ$ , $\gamma$ = 0 $^\circ$ ). Dotted: at 1.5 $\mu$ m; solid: at 630nm. The ordinate gives Universal Time (UT) in hours. All cross talk entries are normalized with the total intensity transmission $\cal T$ (1,1) ( upper left) and are given in %.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2935fig1.eps} \end{figure}$	Figure 1: Beam geometry of the VTT (sketch not to scale). The coelostat consists of two flat aluminum-coated mirrors (C1 and C2), which feed the light beam into the telescope. M3 is the imaging mirror (f=46 m). M4 folds the light down to the laboratories. E1 and E2 are the entrance and exit windows of the evacuated tube. The Instrument Calibration Unit (ICU) is located below the exit window.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2935fig2.ps} \end{figure}$	Figure 2: Response of the telescope proper to linearly polarized light at 630 nm, as the telescope calibration unit was rotated by 180 $^\circ$ in steps of 10 $^\circ$ . From top to bottom the four Stokes parameters are shown for 5 different times during the day.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2935fig3.ps} \end{figure}$	Figure 3: For three wavelengths (518/630/777 nm), the Mueller matrix entries $\cal M$ (1,1), $\cal M$ (1,2), $\cal M$ (1,3), $\cal M$ (2,3), and $\cal M$ (3,3) ( top to bottom) of a mirror sample were measured as function of the angle of incidence, i. The measurements could be reproduced using the refractive indices given in the uppermost panel.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2935fig4.ps} \end{figure}$	Figure 4: The daily variation of the continuum polarization at 630 nm induced by the telescope on July 28, 2003 with C1 at $\gamma =0^{\circ }$ . The solid curve corresponds to the prediction of the telescope model with n=1.41 and k=7.6.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2935fig5.ps} \end{figure}$	Figure 5: Same as Fig. 4 for an observation of a sunspot on August 9, 2003, from UT 9:30 to 10:30.
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