Velocity–distance profile for the region encompassing Andrews-Lindsay 1. The trend predicted from a simple model for Galactic rotation is denoted by the solid line, whereas Cepheids were used to delineate the empirical profile (e.g., Berdnikov et al. 2000). The predicted relation is generally consistent with the observations, where nearer objects exhibit negative velocities and distant targets feature positive velocities. The spatial and kinematic agreement between the remote PN PHR 1315-6555 and the cluster Andrews-Lindsay 1 imply the former is probably a cluster member.