Corrections for the spin parameter in the galaxy sample. Both panels (left and right) are coloured by the ratio (r) of the galaxy angular size to the PSF, given by the major-axis R^maj and σ_PSF, respectively. The ratio r is a parameter that quantifies how well-resolved a galaxy is. Left: generalized Moffat and empirical f_n functions as correction indicators from Graham et al. (2018) and their dependence on the observed (measured) stellar spin parameter, the galaxy angular size, and the width of the PSF. The shaded part of the plot indicates the region where the galaxy spin parameter correction is not physical, leading to ${\lambda }_R^{\mathrm{true}}>1$. Thus, for galaxies with r > 1, no seeing correction is applied. Triangles and circles indicate uncorrected and corrected galaxies, respectively. Triangles can be interpreted as lower limit values. Right: comparison between the observed and intrinsic angular momentum as a function of the galaxy Sérsic index for the corrected galaxies. Solid lines indicate the predicted behaviour of the corrections as a function of the Sérsic index for the mean r values of the respective subsets.