Stellar population of the Rosette Nebula and NGC 2244

Context. Measurements of internal dynamics young clusters and star-forming regions are crucial to fully understand the process their formation. A basic prerequisite for this is a well-established robust list probable members. Aims. In work, we study 2.8° ×2.6° region in emblematic Rosette Nebula, centred cluster NGC 2244, with aim constructing most reliable candidate member date. Using obtained catalogue, can determine various structural kinematic parameters, which help draw conclusions about past future region. Methods. We constructed catalogue containing optical mid-infrared photometry, as well accurate positions proper motions from Gaia EDR3 sources field Nebula. applied probabilistic random forest algorithm derive membership probability each source within our view. Based on almost 3000 members, third concentrated radius 20′ centre identified clustered stellar concentrations region, estimated average distance entire at 1489 ± 37 pc, 1440 32 pc 1525 36 2237. The masses, extinction, ages were derived by fitting spectral energy distribution atmosphere evolutionary models, dynamic was assessed via relative mean motion 2244. Results. 2244 showing clear expansion pattern, an velocity that increases radius. Its initial mass function (IMF) represented two power laws (d N /d M ∝ − α ), slopes = 1.05 0.02 range 0.2–1.5 ⊙ 2.3 0.3 1.5–20 , it agreement detected other regions. age HR diagram, ∼2 Myr. find evidence difference between associated molecular cloud, appears slightly younger. dispersion above virial total (1000 70 ) half-mass (3.4 0.2 pc). From comparison numerical simulations, conclude may be unbound possibly have even formed super-virial state.