Examples of morpho-dynamical models obtained in Mercier et al. (2022) and used in this analysis. For each sub-figure and from top to bottom we have the HST image, the MUSE-HUDF model, and the residuals in the leftmost column, the velocity field map extracted with CAMEL, the best-fit MocKinG velocity field, and the residuals in the middle column, and the raw velocity dispersion map extracted with CAMEL, the beam-smearing model from MocKinG, and the beam-smearing corrected velocity dispersion map from MocKinG in the rightmost column. The top left sub-figure shows a galaxy with a seemingly correct dynamical model, the top right one shows a low S/N galaxy without any velocity gradient in its velocity field map that was flagged, the bottom left one shows a low S/N galaxy with a weak but non-negligible velocity gradient that was not flagged, and the bottom right one shows a massive galaxy with a kinematically disturbed velocity field that was flagged as well.