Aims.We derive accurate parameters related to the CMD, structure and dynamical state of M 52 and
NGC 3960, whose fields are affected by differential reddening. Previous works estimated their
ages in the ranges 35−135 Myr and 0.5−1.0 Gyr, respectively.
Methods.J, H and Ks 2MASS photometry with errors <0.2 mag is used to build CMDs, radial density
profiles, luminosity and mass functions, and correct for differential reddening. Field-star
decontamination is applied to uncover the cluster's intrinsic CMD morphology, and colour–magnitude
filters are used to isolate stars with high probability of being cluster members.
Results.The differential-reddening corrected radial density profile of M 52 follows King's law with core
and limiting radii of Rcore=0.91± 0.14 pc and Rlim=8.0 ± 1.0 pc.
NGC 3960 presents an excess of the
stellar density over King's profile (Rcore=0.62 ± 0.11 pc and Rlim=6.0 ± 0.8 pc)
at the center. The tidal radii of M 52 and NGC 3960 are Rtidal=13.1 ± 2.2 pc and Rtidal=10.7 ± 3.7 pc.
Cluster ages of M 52 and NGC 3960 derived with Padova isochrones are constrained to 60 ± 10 Myr and 1.1 ± 0.1 Gyr.
In M 52 the core MF (χcore=0.89± 0.12) is flatter than the halo's
(χhalo=1.65 ± 0.12). In NGC 3960 they are χcore=−0.74 ± 0.35 and χhalo=1.26 ± 0.26.
The mass locked up in MS/evolved stars in M 52 is ~1200 M⊙, and the total mass (extrapolated to 0.08M⊙)
is ~3800 M⊙. The total mass in NGC 3960 is ~1300 M⊙.
Conclusions.Compared to open clusters in different dynamical states studied with similar methods, the core and
overall parameters of M 52 are consistent with an open cluster more massive than 1000 M⊙ and
~60 Myr old, with some mass segregation in the inner region. The core of NGC 3960 is in an advanced dynamical state with
strong mass segregation in the core/halo region, while the somewhat flat overall MF (χ≈1.07) suggests low-mass
star evaporation. The excess stellar density in the core may suggest post-core collapse. The dynamical evolution of NGC 3960 may have
been accelerated by the tidal Galactic field, since it lies ≈0.5 kpc inside the Solar circle
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