Comparison between the interferometric observables extracted from the MYTHRA averaged images (in blue) and the VLTI/MATISSE data of 3 Puppis (in green), shown respectively in the L-band (first row ), in the M-band ( second row ), and in the N-band ( third row ). Left column : squared visibility amplitudes as a function of spatial frequency in logarithmic scale. Central column : closure phases as a function of spatial frequency, computed using the longest baseline. Right column : final averaged images resulting from MYTHRA, normalised to unity (i.e. the sum over all pixels equals one), with a logarithmic colour scaling, and not convolved with the interferometric beam. The minimum value for each brightness scaling is set to half the standard deviation of the associated image to filter out the artefact produced by the MiRA algorithm.