Current-day position (top ten) and velocity (bottom ten) distribution of the members projected on the galactic plane. The green arrows show what a cluster’s velocity components would be if its radial velocity were larger by 3 km s⁻¹ and therefore indicate the line-of-sight directions for each cluster. From the fact that the clusters appear to be strongly elongated along the line of sight in velocity space while not being visibly elongated in position space, it is apparent that the radial velocity uncertainty is much larger than the uncertainties of other phase space coordinates. Blanco 1 is at a very high galactic latitude, so the apparent cluster elongation in velocity space is mostly along the W axis and is not prominent in the U − V plot.