Fig. 4.
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Phase of the cross-spectrum as function of the spatial frequency for three observing sequences. The observed regions are at the center of the solar disk and the spectrograph slit is oriented along the west-east axis. The straight lines show linear fits of the phase at spatial frequency smaller than 0.6 arcsec−1. Upper panel: cross-spectrum phase of the reference image and image at line cord 16. Lower panel: same for line cord 18.
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