Notes. All of the angular velocities are given in units of the solar angular velocity, Ω_⊙, which we define as the Carrington rotation rate of 2.67 × 10^-6 rad s^-1. As described in the text, the first two distributions are constructed by combining measured rotation periods from different clusters with approximately identical ages. Both of these aggregate clusters are shown in Fig. 2. For each cluster, we bin the stars by mass assuming a bin width of 0.2 M_⊙ and calculate for each mass bin, the number of stars in each bin, n_⋆, the mean angular velocity, , the standard deviation in the angular velocity, σ_Ω, and the 10th, 50th, and 90th percentiles of the distributions, given by Ω₁₀, Ω₅₀, and Ω₉₀ respectively. The values marked as “All” are calculated from all stars with masses between 0.4 M_⊙ and 1.1 M_⊙. The errors on the percentiles are calculated using the bootstrap method. We do not report statistics for NGC 6811 below the highest mass bin because very few stars lie below 0.9 M_⊙.