Properties of Stellar Clusters around High-Mass Young Stars

Abstract

[Abridged] Twenty-six high-luminosity IRAS sources believed to be collection of stars in the early phases of high-mass star formation have been observed in the NIR (J, H, K) to characterize the clustering properties of their young stellar population and gain insight into the initial conditions of star formation in these clusters (Initial Mass Function [IMF], Star Formation History [SFH]), and to deduce mean values for cluster ages. K luminosity functions (KLFs) are compared with simulated ones from a model that generates populations of synthetic clusters starting from assumptions on the IMF, the SFH, and the Pre-MS evolution, and using the average properties of the observed clusters as boundary conditions Twenty-two sources show evidence of clustering from a few up to several tens of objects, and a median cluster radius of 0.7 pc. A considerable number of cluster members present an infrared excess characteristic of young Pre-Main-Sequence objects. We find that the median stellar age ranges between 2.5 10^5 and 5 10^6 years, with evidence of an age spread of the same entity within each cluster. We also find evidence that older clusters tend to be smaller in size, in line with the fact that our clusters are on average larger than those around relatively older Herbig Ae/Be stars. The relationship of the mass of the most massive star in the cluster with both the clusters richness and their total stellar mass suggest that our modeled clusters may not be consistent with them resulting from random sampling of the IMF. Our results are consistent with a star formation which takes place continuously over a period of time which is longer than a typical crossing time.