Structural parameters of 389 local open clusters

Context. The distribution of member stars in the surroundings an open cluster (OC) can shed light on process its formation, evolution, and dissolution. analysis structural parameters OCs as a function their age position Galaxy constrains theoretical models evolution. Gaia catalog is very appropriate for finding members at large distance from centers. Aims. We revisit membership lists solar vicinity, particular, by extending these to peripheral areas through EDR3. then take advantage new study morphological properties mass segregation levels clusters. Methods. used clustering algorithm HDBSCAN parallaxes proper motions systematically search up 50 pc fit King’s radial density profile clusters Gaussian mixture model (GMM) two-dimensional shape. also evaluated degree correlations with Galactic Results. Our method performs well 389 out 467 we selected, including several recently discovered that were poorly studied until now. report detection vast coronae around almost all 71 tidal tails. This multiplies number structures are identified more than four. size cores smaller old young ones average. Moreover, overall seems increase slightly age, but fraction halo decrease. As expected, pronounced oldest clusters, no clear trend evident. Conclusions. extended previously regardless age. decrease proportion populating halos highlights different evaporation processes short timescales they need affect Reported such sizes or depend ages, cannot be described single functions time.