Left: Hα equivalent width vs T_eff for class II (filled dots) and class III (open dots) objects (red, green, and blue mark the position of full, transitional, and substructured disks, respectively). The dashed line defines the threshold above which most probable accretors are positioned at given spectral types, according to White & Basri (2003). Right: Hα flux vs T_eff for the same objects. The dashed line represents the dividing line that was empirically defined by Frasca et al. (2015) as the upper boundary of the chromospheric flux.