SIMBAD references

We present strong evidence that mass segregation in the young open cluster NGC 2422 (age ≈84 Myr) is primarily driven by tidal stripping. Analysis of the radial mass distribution reveals a significant overabundance of low-mass stars (M < 0.85 M_⊙) preferentially located near and beyond the cluster's tidal radius (r_t = 14.4 pc), a hallmark of ongoing tidal stripping. This spatial signature is corroborated by kinematic evidence: the cluster's outskirts exhibit an elevated velocity dispersion (σ_3d = 14.9 km s^–1, F-test p < 0.001) and strong radial anisotropy (β = 0.94 ±0.4), both classic signatures of tidal influence. The cluster's age is significantly greater than its half-mass relaxation time (t_rh = 44.2 Myr), confirming it is dynamically evolved. Crucially, binary stars show no significant radial segregation from single stars (KS-test p ≈ 0.51), ruling them out as the primary driver. Collectively, these results establish tidal stripping as the dominant mechanism currently reshaping the structure and stellar content of NGC 2422.