Chromospheric holes. Observed ALMA 1.25 mm brightness temperature (panels a1 and b1) and synthetic images corresponding to the IRIS+ALMA fit in Fig. 3 (panels a2 and b2), and with an increased number of nodes (panels a3 and b3) for the two regions enclosed by the dashed boxes in Fig. 3. The errorbars on the colormaps indicate the median and the range between the 16th and 84th percentiles. We show part of the observed and synthetic IRIS spectra and the respective inverted gas temperatures and normalized response functions (1.25 mm) at three selected locations as indicated by the different markers for both regions (a and b).
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