Distribution of surface equatorial velocities in a cluster at three different ages (first column: 10 Myr, second column: 100 Myr, and third column: 1 Gyr). Top row (panels a), b), c)): Z_⊙ cluster with the initial velocity distribution from Huang et al. (2010, see their Fig. 6). Second row (panels d), e), f)): same as above, but at Z = 0.002. Third row (panels g), h), i)): same as top row, but with the initial velocity distribution from Huang & Gies (2006). Bottom row (panels j), k), l)): same as top row but for a total number of stars of 400 instead of 10 000.