At the moment we cannot derive a reliable cluster radial profile nor a half-mass radius, or even be certain about the position of the center of the cluster, because our optical observations are incomplete in the vicinity of the early-type stars of NGC 1980, and we only have a “pie-slice” view of the radial extent of the cluster. This should be improved in follow-up work, in particular in combination with dedicated near-infrared observations, which are less sensitive to the strong brightness contrasts between early- and late-type stars in this cluster.