G. G. Sacco, L. Spina, S. Randich, F. Palla, R. J. Parker, R. D. Jeffries, R. Jackson, M. R. Meyer, M. Mapelli, A. C. Lanzafame, R. Bonito, F. Damiani, E. Franciosini, A. Frasca, A. Klutsch, L. Prisinzano, E. Tognelli, S. Degl'Innocenti, P. G. Prada Moroni, E. J. Alfaro, G. Micela, T. Prusti, D. Barrado, K. Biazzo, H. Bouy, L. Bravi, J. López-Santiago, N. J. Wright, A. Bayo, G. Gilmore, A. Bragaglia, E. Flaccomio, S. Koposov, E. Pancino, A. Casey, M. T. Costado, P. Donati, A. Hourihane, P. Jofré, C. Lardo, J. Lewis, L. Magrini, L. Monaco, L. Morbidelli, S. G. Sousa, C. Worley, S. Zaggia
Investigating the physical mechanisms driving the dynamical evolution of young star clusters is fundamental to our understanding of the star formation process and the properties of the Galactic field stars. The young (similar to 2 Myr) and partially embedded cluster Chamaeleon I is one of the closest laboratories for the study of the early stages of star cluster dynamics in a low-density environment. The aim of this work is to study the structural and kinematical properties of this cluster combining parameters from the high-resolution spectroscopic observations of the Gaia-ESO Survey with data from the literature. Our main result is the evidence of a large discrepancy between the velocity dispersion (sigma(stars) = 1.14 +/- 0.35 km s(-1)) of the stellar population and the dispersion of the pre-stellar cores (similar to 0.3 km s(-1)) derived from submillimeter observations. The origin of this discrepancy, which has been observed in other young star clusters, is not clear. It has been suggested that it may be due to either the e ff ect of the magnetic field on the protostars and the filaments or to the dynamical evolution of stars driven by two-body interactions. Furthermore, the analysis of the kinematic properties of the stellar population puts in evidence a significant velocity shift (similar to 1 km s(-1)) between the two subclusters located around the north and south main clouds of the cluster. This result further supports a scenario where clusters form from the evolution of multiple substructures rather than from a monolithic collapse. Using three independent spectroscopic indicators (the gravity indicator gamma, the equivalent width of the Li line at 6708 angstrom, and the H alpha 10% width), we performed a new membership selection. We found six new cluster members all located in the outer region of the cluster, proving that Chamaeleon I is probably more extended than previously thought. Starting from the positions and masses of the cluster members, we derived the level of substructure Q, the surface density Sigma, and the level of mass segregation Lambda(MSR) of the cluster. The comparison between these structural properties and the results of N-body simulations suggests that the cluster formed in a low-density environment, in virial equilibrium or a supervirial state, and highly substructured.
stars: kinematics and dynamics; stars: pre-main sequence; open clusters and associations: individual: Chamaeleon I; techniques: spectroscopic
Astronomy and Astrophysics
Volume 601, Article Number A97