Properties of the variable stars (red crosses) are compared with the entire proper motion (PM) selected cluster members (black circles) from all the open clusters listed in Table 1, along with the corresponding PARSEC isochrones (blue lines). For each figure: Top panels show the PM distributions in the RA–Dec plane (left), the near-IR color–color diagram (middle), and the optical–near-IR color–color diagram (right). Bottom panels display the optical–near-IR color–magnitude diagram (CMD) (left), the near-IR CMD from VVVX survey (middle), and the optical CMD from Gaia DR3 (right). Figures (9) and (10) present the same dataset for IC 2395, but use different isochrones for comparison. Figures (16) and (17) correspond to the same cluster with data from the Gaia survey and VVV, respectively. Figures (22) and (23) compare two datasets of OSCN151, each adopting different proper motions (PM), resulting in variations in the derived data.