Discarded RRL stars (purple star) and cluster members (light gray) are shown, from left to right, in the plane of proper motions (pmDec versus pmRA), parallax, Gaia CAMD and Period-Amplitude diagram. In the CAMD, the solid lines correspond to IS limits from Marconi et al. (2015); the dotted line shows the expected location of the HB at each cluster’s metallicity from Garofalo et al. (2022), and the absolute magnitude and intrinsic colours computed based on the distance and extinction according to Hunt & Reffert (2024); the shading represents the uncertainty in the HB luminosity corresponding to ∆[Fe/H] = 0.5 dex. The star’s ID from Table A.1 and the cluster’s name are shown in the fourth panel top right corner and Y axis, respectively.