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dc.contributor.authorBonatto, Charles Josept_BR
dc.contributor.authorSantos Junior, Joao Francisco Coelho dospt_BR
dc.contributor.authorBica, Eduardo Luiz Damianipt_BR
dc.date.accessioned2014-07-31T02:05:08Zpt_BR
dc.date.issued2006pt_BR
dc.identifier.issn0004-6361pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/98976pt_BR
dc.description.abstractWe use J, H and KS 2MASS photometry to study colour–magnitude (CMDs) and colour–colour diagrams, structure and mass distribution in the ionizing open cluster NGC 6611. Reddening variation throughout the cluster region is taken into account followed by field-star decontamination of the CMDs. Decontamination is also applied to derive the density profile and luminosity functions in the core, halo and overall (whole cluster) regions. The field-star decontamination showed that the lower limit of the main sequence (MS) occurs at ≈5 Mʘ. Based on the fraction of KS excess stars in the colour–colour diagram we estimate an age of 1.3 ± 0.3 Myr which is consistent with the presence of a large number of premain sequence (PMS) stars. The distance from the Sun was estimated from known O V stars in the cluster area and the turn-on stars connecting the PMS and MS, resulting in dʘ = 1.8 ± 0.5 kpc. The radial density distribution including MS and PMS stars is fitted by a King profile with a core radius Rcore = 0.70 ± 0.08 pc. The cluster density profile merges into the background at a limiting radius Rlim = 6.5 ± 0.5 pc. From the field-star subtracted luminosity functions we derive the mass functions (MFs) in the form ø(m) ∝ m−(1+χ). In the halo and through the whole cluster the MFs have slopes χ = 1.52 ± 0.13 and χ = 1.45 ± 0.12, respectively, thus slightly steeper than Salpeter’s IMF. In the core the MF is flat, χ = 0.62 ± 0.16, indicating some degree of mass segregation since the cluster age is a factor ~2 larger than the relaxation time. Because of the very young age of NGC6611, part of this effect appears to be related to the molecular cloud-fragmentation process itself. We detect 362 ± 120 PMS stars. The total observed mass including detected MS (in the range 5−85 Mʘ) and PMS stars amounts to ~1600 Mʘ, thus more massive than the Trapezium cluster. Compared to older open clusters of different masses, the overall NGC 6611 fits in the relations involving structural and dynamical parameters. However, the core is atypical in the sense that it looks like an old/dynamically evolved core. Again, part of this effect must be linked to formation processes.en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofAstronomy and astrophysics. Les Ulis. Vol. 445, no. 2 (Jan. 2006), p. 567-577pt_BR
dc.rightsOpen Accessen
dc.subjectEstrelas variaveispt_BR
dc.subjectGalaxy: open clusters and associations: individual: NGC6611en
dc.subjectGalaxy: structureen
dc.titleMass functions and structure of the young open cluster NGC 6611pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000538114pt_BR
dc.type.originEstrangeiropt_BR


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