Mass accretion rate as a function of stellar mass for the Lupus sample of Alcalá et al. (2017) after revisiting the stellar and accretion parameters adopting the Gaia DR2 distances. The transitional discs are shown with red crossed squares. The average errors in log M_⋆ and log Ṁ_acc are shown in the upper left. The symbols corresponding to MY Lup, SST c2dJ160830.7-382 827 and RY Lup, the latter also investigated with HST (Arulanantham et al. 2018), are labelled. The big red dot represents the corrected value of Ṁ_acc for the former, with the vertical red line indicating the corresponding vertical shift. The other three objects classified as weak ornegligible accretors (see Sect. 1) are plotted with plus symbols and are also labelled. Sub-luminous objects are not plotted. The black dashed line shows the double power law theoretically predicted by Vorobyov & Basu (2009), and the continuous magenta lines represent the fits to the data as in Eqs. (4) and (5) of Alcalá et al. (2017); the long-dashed blue line shows the robust double-linear fit following the prescription by Manara et al. (2017a).