Valid measurements of pEW(He IR) as function of pEW(Hα) for different spectral types as given in legend. The dashed vertical line marks the dividing line between active (Hα in emission) and inactive stars (Hα in absorption) for both panels. The cloud of inactive late-type M dwarfs (right) connects smoothly to the cloud of the inactive early-type M dwarfs (left) shifting to lower maximum values for later spectral types. For better comparison, we show spectral type M2/M2.5 in both panels.