  We present a new technique for estimating the distance to young open
clusters. The method requires accurate measurement of the axial rotation period
of late-type members of the cluster: rotation periods are first combined with
projected rotation velocities and an estimate of the angular diameter for each
star -- obtained using the Barnes-Evans relation between colour and surface
brightness. A 'best' cluster distance estimate is then determined using
standard techniques from the theory of order statistics which are in common use
in the general statistics literature. It is hoped that this new method will
prove a useful adjoint to more traditional distance methods, and will provide a
better %determination of the distance scale within the solar neighbourhood.
(Figures / preprint available on request)
