Fig. 3
Top panel: current distribution of spectral types in the PMS and expected distribution when the stars reach the MS, asindicated in the legend. The error bars reflect the uncertainties on the spectral types. Bottom panel: number of HAeBes vs. stellar mass. The error bars for the number of stars per bin considering the uncertainties in M* are indicated. The dashed red line corresponds to the IMF (Salpeter 1955) normalized to the bin 2–3 M⊙. Stars with masses >12 M⊙ have been grouped together for simplicity.
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