Near-IR imaging of Galactic massive clusters: Westerlund 2

J. Ascenso, J. Alves, Y. Beletsky, M. T. V. T. Lago

Resumo
Context. Most stars in the Galaxy were formed in massive clusters. To understand nature’s favorite mode of star formation and the initial stages of the life of most stars one needs to characterize the youngest and resolved massive clusters in the Milky Way. Unfortunately young massive clusters are challenging observational targets as they are rare, hence found at large distances, are still embedded in their parental molecular cloud, and are swamped by relatively bright nebulae.
Aims. In this paper we propose to use deep subarcsec resolution NIR data to derive the basic parameters of the unstudied population of massive cluster Westerlund 2.
Methods. We present deep JHK_s images (~0.6” seeing) and photometry of Westerlund 2. This is the most complete photometric census of the cluster’s population to date.
Results. We detect a total of 4701, 5724, and 5397 sources in the J, H, and K_s bands respectively. By comparison with main-sequence and pre-main-sequence model tracks we determine an average visual extinction toward the cluster of 5.8 mag, a likely distance of 2.8 kpc, and an age of 2.0 ± 0.3 Myr for the core of the cluster. Although we have the sensitivity to reach beyond the Hydrogen burning limit in the cluster we are only complete to about 1 M_solar due to source confusion. We find no evidence for a top-heavy MF, and the slope of the derived mass function is −1.20 ± 0.16. Based on the extrapolation of a field IMF, we roughly estimate the total mass of the cluster to be about 10⁴ M_solar. We find compelling evidence for mass segregation in this cluster.

Palavras chave
open clusters and associations: individual: Westerlund 2 – stars: pre-main sequence – infrared: stars

Notas
The tables with the photometry (Table 2) are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/466/137

Astronomy and Astrophysics
Volume 466, Página 137
abril 2007

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