Fig. 12

Count profiles of spectral images of a star, α And (Alpheratz). The solid line profile was obtained for the star images that appeared in the video frames’ central part (No. 5 in Fig. 14). The blue broken line profile was obtained for the images near the edge of the frames (No. 6 in Fig. 14). One hundred frames were averaged for each profile. We converted the positions in a spectral image to wavelengths and showed them in the abscissa. The dark frame has been subtracted. We did not apply the correction for the atmospheric dispersion because the star was close to the zenith. The correction for the 2nd-order images was made. We did not make the corrections for the atmospheric transmittance