Spatial and dynamical structure of the NGC 2264 star-forming region

Context. The formation of stars within molecular clouds and the early stages of stellar evolution (e.g., mass accretion and disk dispersal) are all active research topics. The target of this study, NGC 2264, is a benchmark star-forming region in which these issues can be profitably studied.
Aims: We revisit the structure, dynamics, and star-forming history of NGC 2264 in order to advance our understanding of the processes that lead from molecular clouds to protostars, stellar associations, and the evolution of both.
Methods: We assembled a new extensive sample of NGC 2264 members. To this end we used new X-ray data obtained with the XMM-Newton telescope, Gaia eDR3 data, and an extensive collection of public and published catalogs. Following a previous suggestion that the star-forming region might extend significantly beyond the better studied areas, our search covers a wide 2.5×2.5 degrees region in the sky.
Results: Our catalog comprises more than 2200 candidate members, which is a ∼100% increase over previous determinations. We analyze their spatial distribution and define new substructures. Using Gaia parallaxes we estimate a new average distance to NGC 2264 of 722±2 pc and suggest that the embedded Spokes subregion is ∼20 pc farther away within the molecular cloud. A complex dynamics is unveiled by the available proper motions and radial velocities: we observe signs of global expansion and rotation. At the same time, we observe the collapse and coalescence of two substructures in a region where active star formation is taking place. The fraction of stars with disks and of those undergoing circumstellar accretion varies significantly across the field, suggesting that star formation has been occurring for several million years. A particularly low accretion disk fraction around the O VII star S Mon might be attributed to external disk photoevaporation or to an older age of the stars in the region.
Conclusions: NGC 2264 is not dynamically relaxed and its present configuration is the result of multiple dynamical processes. The cloud has been forming stars for several million years and we identify the process that is likely responsible for the ongoing formation activity.

Full Tables 2, 3, A.1 are only available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/670/A37