We performed a statistical study of two old open clusters NGC 188 and M 67 using Gaia DR3 data. No tidal tails of the clusters were detected, which most likely had been destroyed when the cluster passed through the Galactic plane. The size estimates of the clusters depend on the range of astrometric parameters and stellar magnitudes of the stars used for star counts. The mass spectra of two clusters differ significantly. NGC 188 shows a deficit of low-mass stars compared to M 67. In the halo region of NGC 188 (compared to the core region of the cluster), there is a relative excess of the low-mass stars (just as in the case of M 67) and a deficit of stars in the mass range from 0. 66 to 0. 9 solar masses. Comparison with the Hunt and Reffert samples showed that almost all the stars from these samples are contained among the stars we selected for counting. Moreover, the group probability of these stars belonging to clusters, estimated by the uniform field method, is higher than 60%. It is shown that the velocity dispersion of single stars (selected according to the stellar magnitude–color index diagrams) is significantly smaller than the velocity dispersion of unresolved binary stars. The work is partially based on a talk presented at the Modern Stellar Astronomy 2025 conference.
Seleznev et al. (Mon,) studied this question.