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Stellar kinematics is a powerful tool for understanding the formation processof stellar associations. Here, we present a kinematic study of the youngstellar population in the Rosette nebula using the recent Gaia data andhigh-resolution spectra. We first isolate member candidates using the publishedmid-infrared photometric data and the list of X-ray sources. A total of 403stars with similar parallaxes and proper motions are finally selected asmembers. The spatial distribution of the members shows that this star-formingregion is highly substructured. The young open cluster NGC 2244 in the centerof the nebula has a pattern of radial expansion and rotation. We discuss itsimplication on the cluster formation, e.g., monolithic cold collapse orhierarchical assembly. On the other hand, we also investigate three groupslocated around the border of the H II bubble. The western group seems to bespatially correlated with the adjacent gas structure, but their kinematics isnot associated with that of the gas. The southern group does not show anysystematic motion relative to NGC 2244. These two groups might be spontaneouslyformed in filaments of a turbulent cloud. The eastern group is spatially andkinematically associated with the gas pillar receding away from NGC 2244. Thisgroup might be formed by feedback from massive stars in NGC 2244. Our resultssuggest that the stellar population in the Rosette Nebula may form throughthree different processes: the expansion of stellar clusters, hierarchical starformation in turbulent clouds, and feedback-driven star formation.

A kinematic perspective on the formation process of the stellar groups in the Rosette Nebula