Revisiting the old open cluster NGC 2506 based on reliable members

We investigate the structural parameters and dynamical state of the 2Gyr old open cluster NGC 2506 based on more reliable cluster members. We apply a robust clustering method to calculate membership probabilities for more than 8000 sample stars within 90 ' (similar to 81pc) from the cluster center in the Gaia-DR3 catalogue. Based on the membership probabilities, we identify more than 2500 members (including extra-tidal members) which cover a wide range of magnitudes (G similar to 9-20mag). We find that NGC 2506 has a detectable radius of R-cl similar to 40 ' (36pc), and its members extend up to a large radial distance of at least 90 ' (81pc) from the cluster center. We determine the core and tidal radii of the cluster to be R-c = 2.' 69 +/- 0.' 02 (2.4pc) and R-t = 48.' 02 +/- 4.84 (43.3pc), respectively, indicating a high concentration parameter of log(R-t/R-c) similar to 1.3 for the cluster. A Gaussian mixture model and principle component analysis are used to investigate the two-dimensional structural parameters of the cluster. We find that NGC 2506 has a near-circular core (e similar to 0.96) and a slightly elongated halo (e similar to 0.87). In addition, we find evidence for the existence of some extra-tidal members (including some high-mass stars). We also find that some red clump giants inside the tidal radius are located at distances smaller than the mean distance of the cluster, suggesting that they may have escaped from the cluster. Our findings suggest that NGC 2506 is losing its member stars, including high-mass stars. However, no clear tidal tails can be detected around the cluster.