All Figures

$\begin{figure} \par\includegraphics[width=9cm,clip]{9959f01.eps}\end{figure}$ Figure 1: Polarimetry Calibration for 13-Sep.-2007. The lines are theoretical curves fitted to the data recorded for the polarimetric states. The horizontal dotted lines are the LP-only observations, the vertical dashed lines are the fitted angle offset (for 0 $^\circ$ and 180 $^\circ$ ) of the QWP. The accuracy with which the intersection points of the LP-only lines and their corresponding curves line up vertically and how well this matches the fitted offset angle is an indication of the overall accuracy of the fit.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9959f02.eps}\end{figure}$ Figure 2: Instrumental polarization for 12-Sep.-2006 as a function of time. The plotted curves are the model predicted telescope polarization for Q (solid), U (dotted) and V (dashed), the crosses are the actual values measured below the exit window of the telescope.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{9959f03.eps}\end{figure}$ Figure 3: Sunspot AR10908 observed on 12 Sep. 2006 in Fe I 630.25 nm -5 pm. The color scaling saturates at $\pm 15$ % for U/I and Q/I, and at $\pm 25$ % for V/I.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9959f04.eps}\end{figure}$ Figure 4: Schematic drawing of the optical set-up.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9959f05.eps}\end{figure}$ Figure 5: Sketch of the acquisition scheme of a full Stokes MOMFBD data set for 2 line positions. The 2 line positions, $\lambda _0-\Delta \lambda _1$ and $\lambda _0-\Delta \lambda _2$ , were recorded sequentially. For each line position, the LCVRs cycled through 4 states LC0-LC3, changing state for each exposure t. For each narrow-band exposure, a pair of accompanying wide-band phase-diversity images were recorded. The wide-band channel served as an anchor channel for the narrow-band images. For the data sets discussed in this paper, the number of exposures for each line position was 500, i.e., n=500.
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In the text

$\begin{figure} \par\includegraphics[width=9cm]{9959f06.eps}\end{figure}$ Figure 6: Panel a) shows a magnetogram-like image constructed from flatfielded images of the same liquid crystal state. Panel b) shows a similar image constructed from a MOMFBD restoration based on the same images as panel a). Both panel a) and b) have the same scaling, -0.01 to +0.01. Panel c) shows the Fe I 630.2 -5 pm Stokes V magnetogram from the same data set and the same number of images. The scaling is -0.05 to +0.05. Panel d) shows the wide band image of the same region and data set.
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In the text

$\begin{figure} \par\includegraphics[width=9cm]{9959f07.eps}\end{figure}$ Figure 7: Noise in ``fake'' magnetograms as function of number of exposures per state. The solid line is for flatfielded data, similar to panel a) of Fig. 6. Crosses are MOMFBD restored data, similar to panel b) of Fig. 6. The dotted line is the 1/ $\sqrt {n}$ noise behaviour of the photon-noise dominated case with 17 photo-electrons per count. Noise measurements on real -50 mÅ magnetograms: quiet Sun Stokes V only (asterisks), Stokes Q close to the sunspot of 12-Sep.-2006 (diamonds), Stokes U disk center from 2007 (triangles).
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In the text

$\begin{figure} \includegraphics[bb= 0 0 500 162, clip, width=18cm]{9959f08.eps}\end{figure}$ Figure 8: Panel a) shows a part of a Fe I 630.2 -5 pm Stokes I image, observed on 12-Sep-2006, MOMFBD restored based on 110 exposures per state. Panel b) shows the corresponding MOMFBD restored stokes V image. Panel c) is a Stokes V image constructed from the flat-fielded data. Panels b) and c) have the same scaling, -0.2 to 0.2. The graph in panel d) shows power spectra of part of the MOMFBD restored wide-band image (solid line), the MOMFBD restored Stokes I image (dotted), and the flat-fielded Stokes I image (dash-dotted line). The vertical long-dashed line marks the theoretical diffraction limit $\lambda$ /D of 0 $.\!\!^{\prime\prime}$ 134 at this wavelength.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=4.4cm,clip]{9959f09a.eps}\includegraphics[width=4.4cm,clip]{9959f09b.eps} } \end{figure}$ Figure 9: Scatter plots of relative difference comparing Stokes V magnetograms restored with different number of wavefront modes. Panel a) compares a 2-mode with a 34-mode restoration, b) compares a 256-mode with a 34-mode restoration. For the densest scatter regions, density contours are plotted to avoid crowding.
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In the text

$\begin{figure} \includegraphics[width=18cm,clip]{9959f10a.eps}\par\includegraphi... ...ip]{9959f10c.eps}\par\includegraphics[width=18cm,clip]{9959f10d.eps}\end{figure}$ Figure 10: Dark-cored penumbral filaments observed in two sunspots. Top two rows: AR 10908 on 12 Sep. 2006, bottom rows: AR 10908 on 15 Sep. 2006, with the center-side penumbra on the third row, and the limb-side penumbra on the bottom row. Left to right: maps of Stokes I in +5 pm, total circular polarization, total linear polarization, total polarization, and the ratio of total circular over linear polarization. The arrow in the Stokes I images points towards the center of the solar disk.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{9959f11.eps}\end{figure}$ Figure 11: Faculae observed on 7 Jan. 2006. The left column shows Stokes maps at -5 pm, the middle column at +5 pm. The Stokes maps Q/I, U/I, V/I saturate at $\pm$ 10%. The right column shows from top to bottom: wide-band (WB), total linear polarization (TLP), the ratio of total circular over linear polarization, and a map of the Doppler signal computed from the $\pm$ 5 Stokes I images. The limb direction is towards the top of the figures.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9959f02.eps}\end{figure}$	Figure 2: Instrumental polarization for 12-Sep.-2006 as a function of time. The plotted curves are the model predicted telescope polarization for Q (solid), U (dotted) and V (dashed), the crosses are the actual values measured below the exit window of the telescope.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{9959f03.eps}\end{figure}$	Figure 3: Sunspot AR10908 observed on 12 Sep. 2006 in Fe I 630.25 nm -5 pm. The color scaling saturates at $\pm 15$ % for U/I and Q/I, and at $\pm 25$ % for V/I.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9959f04.eps}\end{figure}$	Figure 4: Schematic drawing of the optical set-up.
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$\begin{figure} \par\mbox{\includegraphics[width=4.4cm,clip]{9959f09a.eps}\includegraphics[width=4.4cm,clip]{9959f09b.eps} } \end{figure}$	Figure 9: Scatter plots of relative difference comparing Stokes V magnetograms restored with different number of wavefront modes. Panel a) compares a 2-mode with a 34-mode restoration, b) compares a 256-mode with a 34-mode restoration. For the densest scatter regions, density contours are plotted to avoid crowding.
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