All Figures

$\begin{figure} \par\includegraphics[height=12.4cm,width=7.5cm,clip]{8642f1.eps}\end{figure}$ Figure 1: Top panel: the solid line displays the Ca II 854.2 nm atlas profile, while the dashed line shows the effects of the 0.46 nm FWHM prefilter utilized in IBIS observations. The actual maximum transmission of the prefilter is 35%. The asterisks indicate the wavelengths of the images in Figs. 2 and 3. Bottom panel: normalized prefilter profile (solid, upper curve) and periodic transmission profile of the combined Fabry Perot's (solid, multiple peaks curve). Note the logarithmic scale. The dashed line indicates the effects of the prefilter on the FPs transmission profile, i.e. the large suppression of the secondary maxima of the curve, as needed to reduce the spectral parasitic light.
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In the text

$\begin{figure} \par\includegraphics[height=14.4cm,width=16.5cm,clip]{8642f2.eps}\end{figure}$ Figure 2: Ca II 854.2 nm data acquired on 2004 May 31. Wavelength runs from left to right, top to bottom, as indicated in the panels, with offsets in pm from the nominal line core. The figure shows a cutout of 64'' $\times$ 41'' of the full circular FOV, originally 80'' in diameter. Each panel was normalized for optimum display. The topmost left panel shows the cospatial, cotemporal broadband image (acquired at 710 nm, FWHM = 10 nm). The bottom right panel gives the cotemporal HR MDI map, scaled between $\pm$ 500 G. The intensity in the far wings of the Ca II 854.2 nm line is strongly sensitive to the presence of magnetic structures (cf. Leenaarts et al. 2006, and Sect. 5.2).
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In the text

$\begin{figure} \par\includegraphics[height=14.4cm,width=16.5cm,clip]{8642f3.eps}\end{figure}$ Figure 3: Same as Fig. 2, for 2004 June 2 data. In the speckle-reconstructed broadband image many bright points can be appreciated in the network areas. The MDI map shows a strong, bipolar network (image scaled between $\pm$ 500 G). Note how the fibrillar structures originating from the network elements, very visible in the inner wings and core images, extend over a substantial fraction of the FOV, different from what occurs in the area depicted in Fig. 2. The two dashed lines in the upper-right panel indicate the positions where the slit spectra of Fig. 6 have been obtained.
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In the text

$\begin{figure} \par\includegraphics[height=7.8cm,width=5.2cm,angle=-90,clip]{864... ...ncludegraphics[height=7.8cm,width=5.2cm,angle=-90,clip]{8642f4b.eps}\end{figure}$ Figure 4: Speckle-reconstructed sample images from the weak plage region of Oct. 1, 2005. Upper panel: image obtained at 65 pm in the blue wing of the line. FOV is about 60'' $\times$ 40''. Bottom panel: corresponding image at 20 pm in the blue wing, obtained 200 s later. Images have been reconstructed applying the speckle code of Wöger (2006). See the online version for a movie of these data.
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In the text

$\begin{figure} \par\includegraphics[height=6.1cm,width=8.4cm,clip]{8642f5.eps}\end{figure}$ Figure 5: Contribution function for Ca II 8542 computed in plane-parallel, hydro-static, average quiet-Sun atmosphere (Fontenla et al. 1993). Height zero refers to the level at which optical depth in the continuum at 500 nm is unity.
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In the text

$\begin{figure} \par\includegraphics[height=7.6cm,width=7.2cm,clip]{8642f6.eps}\end{figure}$ Figure 6: ``Slit'' spectra obtained around the middle of the sequence of 2004 June 2, from two horizontal cuts of the data displayed in Fig. 3. The x-axis is the wavelength distance from the average line core position. The left spectrum corresponds to the upper slice across network areas, while the right one corresponds to the lower slice, and represents quiet internetwork areas.
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In the text

$\begin{figure} \par\includegraphics[height=11.7cm,width=7.8cm,clip]{8642f7.eps}\end{figure}$ Figure 7: Average line profiles for the data acquired on 2004 June 2. Panel a): the spectrum averaged over the whole dataset (thin solid line) is compared to the Liege atlas (thick solid). The effect of the prefilter transmission has been removed from the observations. The profiles averaged over different solar features defined by using an intensity threshold are also shown: network points (dashed), fibrils (dot-dashed), and internetwork (dotted). Panel b): as in panel a), but this time fibrils and internetwork areas were defined using dynamical properties.
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In the text

$\begin{figure} \par\hspace*{3.5mm}\includegraphics[height=5cm,width=6.5cm,clip]{... ...ace*{5mm} \includegraphics[height=5cm,width=6.8cm,clip]{8642f8b.eps}\end{figure}$ Figure 8: Upper panel: line-of-sight velocity distribution for the dataset of 2004 June 2. Solid line: overall FOV and time (more than 2 $\times$ 10⁷ values); dashed, dash-dotted, and dotted: distributions for, respectively, network points, fibrils, and internetwork. Bottom panel: velocity power spectra for the same features (symbols as upper panel). The curves represent an average over the corresponding pixels.
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In the text

$\begin{figure} \par\includegraphics[height=6.1cm,width=8.4cm,clip]{8642f5.eps}\end{figure}$	Figure 5: Contribution function for Ca II 8542 computed in plane-parallel, hydro-static, average quiet-Sun atmosphere (Fontenla et al. 1993). Height zero refers to the level at which optical depth in the continuum at 500 nm is unity.
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$\begin{figure} \par\includegraphics[height=7.6cm,width=7.2cm,clip]{8642f6.eps}\end{figure}$	Figure 6: ``Slit'' spectra obtained around the middle of the sequence of 2004 June 2, from two horizontal cuts of the data displayed in Fig. 3. The x-axis is the wavelength distance from the average line core position. The left spectrum corresponds to the upper slice across network areas, while the right one corresponds to the lower slice, and represents quiet internetwork areas.
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