Fraction of FRs (left) and SRs (right) that populate each accretion class as a function of stellar mass, represented with a cumulative bar plot. The open circles show the fraction of fast or slow rotators in each mass bin. The vertical dashed lines represent the stellar mass bins adopted in the paper. FRs and SRs populate the four accretion classes differently, highlighting the different accretion histories of the two classes, but also that several formation pathways can lead to the formation of a FR or a SR.