Kinematic structure in the young σ Orionis association

We have used precise radial velocity measurements for a large number of candidate low-mass stars and brown dwarfs to show that the young sigma Ori 'cluster' consists of two spatially superimposed components which are kinematically separated by 7 km s(-1) in radial velocity, and which have different mean ages. We examine the relationship of these two kinematic groups to other populations in the Orion OB1 association, and briefly discuss the consequence of mixed age samples for ongoing investigations of the formation and evolution of low-mass objects in this much-observed region.