Rotation period distribution of stars between 0.1 and 1.2 M_⊙ from the 120 Myr Pleiades cluster. The red circles correspond to the stars that display the rotational kink. Data are from Rebull et al. (2016) and Stauffer et al. (2016). The stellar masses are estimated using the absolute K_s magnitudes and the 125 Myr isochrones from Baraffe et al. (2015). The blue and red lines correspond to the least-squares fit to the slowest rotating stars inferred by Stauffer et al. (2016, see their Fig. 2). The rotational distributions are the same as in Fig. 7.