Comparison between measured and modeled normalized intensity profiles, I(r)∕I(r = 0), as a functionof the angular radius r (from 0 to 0.5⊘_H). The interferometrically measured profiles are shown in plain lines for the linear (green) and power-law (black) LD models, fitted to the PIONIER data (see Tables 2 and 3). The dashed red and dotted blue profiles correspond to selected SATLAS stellar atmosphere models computed in spherically symmetric geometry in the H band (Lester & Neilson 2008; Neilson & Lester 2013). The selected models correspond to a 10 M_⊙ model, with T_eff (blue) or log g (red) being closest to the measured values. The measured power-law LD and the SATLAS profiles show a general good agreement, even though they do not exactly match the measured Canopus parameters. A small discrepancy is mostly seen only very close (above 97%) to the stellar limb (see the zoomed-in plot in the inset). The precision of present interferometric data does not allow such tiny differences to be distinguished among these intensity profiles.