Conclusions
few-body decay is likely in early stellar evolution
stellar dynamics approximates the evolution
two-step IMF can reproduce obsvd. trends in BF & MR
cluster decay broadens and reduces scale by 10
velocity distributions are nonGaussian, high vel. Tails
spatial segregation of multiples from singles
field brown dwarfs are single, with significant velocities
Star formation during a paradigm shift from binary to multiple star formation