Produção Nacional
Revisado por pares
Probing the age and structure of the nearby very young open clusters NGC 2244 and 2239
2009; Oxford University Press; Volume: 394; Issue: 4 Linguagem: Inglês
10.1111/j.1365-2966.2009.14474.x
ISSN1365-2966
Autores Tópico(s)Galaxies: Formation, Evolution, Phenomena
ResumoThe very young open cluster (OC) NGC 2244 in the Rosette Nebula was studied with field-star-decontaminated 2MASS photometry, which shows the main-sequence (MS) stars and an abundant pre-MS (PMS) population. Fundamental and structural parameters were derived with colour-magnitude diagrams (CMDs), stellar radial density profiles (RDPs) and mass functions (MFs). Most previous studies centred NGC 2244 close to the bright K0V star 12 Monocerotis, which is not a cluster member. Instead, the near-IR RDP indicates a pronounced core near the O5 star HD 46150. We derive an age within 1--6 Myr, an absorption $\aV=1.7\pm0.2$, a distance from the Sun $\ds=1.6\pm0.2$ kpc ($\approx1.5$ kpc outside the Solar circle), an MF slope $\chi=0.91\pm0.13$ and a total (MS+PMS) stellar mass of $\sim625 \ms$. Its RDP is characterised by the core and cluster radii $\rc\approx5.6\arcmin$ ($\approx2.6$ pc) and $\rl\approx10\arcmin$ ($\approx4.7$ pc), respectively. Departure from dynamical equilibrium is suggested by the abnormally large core radius and the marked central stellar excess. We also investigate the elusive neighbouring OC NGC 2239, which is low-mass ($m_{MS+PMS}\approx301 \ms$), young ($5\pm4$ Myr) rather absorbed ($\aV=3.4\pm0.2$), and located in the background of NGC 2244 at $\ds=3.9\pm0.4$ kpc. Its RDP follows a King-like function of $\rc\approx0.5\arcmin\approx0.5$ pc and $\rl\approx5.0\arcmin\approx5.6$ pc. The MF slope, $\chi=1.24\pm0.06$, is essentially Salpeter's IMF. NGC 2244 is probably doomed to dissolution in a few $10^7$ yr. Wide-field extractions and field-star decontamination increase the stellar statistics and enhance both CMDs and RDPs, which is essential for faint and bright star clusters.
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