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$\begin{figure} \par\includegraphics[width=12cm,clip]{2001F1.eps} \end{figure}$ Figure 1: Reconstructed images of the centre side of the sunspot NOAA9919 on 29.04.2002 in the 6301 Å spectral range. From left to right: broadband image, narrowband image from the outer wings of Fe I 6301.5 Å ("continuum'' image, see Fig. 2), and narrowband image from the line core of the same line. The intensity of theline core image is re-scaled to emphasisethe small-scale fluctuations. The distance of the tickmarks in the lower right corner corresponds to 1 $^{\prime \prime }$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2001F2.eps} \end{figure}$ Figure 2: Temperature response functions for Fe I 6301.5 Å in the penumbra model of del Toro Iniesta et al. (1994). The units of the response functions are erg cm^-2 s^-1 Hz^-1 ster^-1 K^-1 km^-1. Solid curve: continuum response function $RF_{\rm T}$ ; dash-dotted: average from wavelengths in the outer wings; dashed: average from wavelengths around line centre. $\gamma$ is the angle between the magnetic field and the LOS, $\chi$ the azimuth of the magnetic field and $\mu=\cos\theta$ .
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{2001F3.eps} \end{figure}$ Figure 3: Reconstructed images of the sunspot NOAA9919 on 29.04.2002 in the 6301 Å spectral range. Top: limb side part, bottom: centre side; from left to right: broadband images, narrowband images after deconvolution from the outer wings ("continuum''), and from the line core. The distance of the tickmarks is 1 $^{\prime \prime }$ .
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In the text

$\begin{figure} {\includegraphics[width = 7.7cm,bbllx=100pt,bblly=375pt,bburx=590... ...bbllx=100pt,bblly=375pt,bburx=590pt,bbury=770pt] {2001F4c.ps} } \end{figure}$ Figure 4: Speckle-reconstructed broadband images of the sunspot NOAA0346 ( upper panels), its magnetic field strengths $B_{\rm eff}$ ( middle panels) and velocities ( lower panels) determined in Fe II 6149 with the COG method. The magnetic field and velocity maps are padded with an average shade when the signals were too low for a reliable determination (for $B_{\rm eff}$ less than 50 Gauss). Velocities away from the observer are positive and are coded with dark color. The arrow points towards disc centre and the coordinates are in arcsec.
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In the text

$\begin{figure} \vskip +0.02cm {\includegraphics[width = 7.6cm,bbllx=100pt,bblly=... ...,bbllx=100pt,bblly=350pt,bburx=560pt,bbury=775pt] {2001F5d.ps} } \end{figure}$ Figure 5: Speckle reconstructed broadband images of the sunspot NOAA9919 ( upper left panels), its velocities from COG ( lower left panels) and magnetic field strengths $B_{\rm eff}$ from COG ( upper right panels) and from the separation of V extrema ( lower right) in Fe I 6302.5. The magnetogram from the V amplitude separation is padded with zero shade when the signals are too low for a reliable determination. Velocities away from the observer are positive and are coded with dark color and velocity values in the umbral area are set to zero because there the COG method does not yield reliable values. The arrow points towards disc centre and the coordinates are in arcsec.
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In the text

$\begin{figure} \par\resizebox{\hsize}{!} {\includegraphics[width=8.5cm,bbllx=50pt,bblly=355pt,bburx=780pt,bbury=1080pt] {2001F6.ps}} \end{figure}$ Figure 6: Subfield of the disc centre side of the penumbra in Fig. 5 with continuum image ( upper left), 6301.5 line core image ( upper right), velocity map ( lower left) and magnetogram from COG ( lower right). Magnetic field contours (solid) at a level of 1200 Gauss and contours surrounding magnetic features (dashed) are overlaid. The longer tickmarks are at 1 $^{\prime \prime }$ distance.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{2001F3.eps} \end{figure}$	Figure 3: Reconstructed images of the sunspot NOAA9919 on 29.04.2002 in the 6301 Å spectral range. Top: limb side part, bottom: centre side; from left to right: broadband images, narrowband images after deconvolution from the outer wings ("continuum''), and from the line core. The distance of the tickmarks is 1 $^{\prime \prime }$ .
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