log(Ṁ) derived from the Hα_10% following the Natta et al. (2004) as a function of the FWZI for the good cases with Hα line in emission, the confident accretors, with high S/N (> 40), and Hα_10% >  200 km s⁻¹, whose spectra are not altered by the nebular contribution and therefore allow us to derive reliable measurements from their peak. The data of the good cases are shown as lilac dots and the best-fit line is superimposed.