We show the T_eff–﹩v\sin i﹩ distribution of BSSs in open clusters (upper panel, in red, from Figure 2) and low-density globular clusters (lower panel, in blue). Like in Figure 3, using MIST evolutionary tracks, we calculated the equatorial velocity for stars that are halfway through their main-sequence lifetimes at a specific T_eff with rotational periods of 2 and 4 days, and plot these with dashed lines. We further show the BSS Kraft break at solar metallicity (red area) in the upper panel and the best-fit T_eff with errors (blue line) that demarcates a transition of the globular cluster BSS rotation distribution in the lower panel.