EDP Sciences
Free Access
Volume 445, Number 2, January II 2006
Page(s) 567 - 577
Section Galactic structure, stellar clusters and populations
DOI https://doi.org/10.1051/0004-6361:20052793

A&A 445, 567-577 (2006)
DOI: 10.1051/0004-6361:20052793

Mass functions and structure of the young open cluster NGC 6611

C. Bonatto1, J. F. C. Santos Jr.2 and E. Bica1

1  Universidade Federal do Rio Grande do Sul, Instituto de Física, CP 15051, Porto Alegre 91501-970, RS, Brazil
    e-mail: charles@if.ufrgs.br
2  Universidade Federal de Minas Gerais, ICEx, Departamento de Física, CP 702, Belo Horizonte 30162-970, MG, Brazil

(Received 31 January 2005 / Accepted 9 September 2005 )

We use J, H and $K_{\rm S}$ 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 $\approx$ $5\,\mbox{$M_\odot$ }$. Based on the fraction of $K_{\rm S}$ excess stars in the colour-colour diagram we estimate an age of $1.3\pm0.3$ Myr which is consistent with the presence of a large number of pre-main 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 $\mbox{$d_\odot$ }=1.8\pm0.5\,\rm kpc$. The radial density distribution including MS and PMS stars is fitted by a King profile with a core radius $\mbox{$R_{\rm core}$ }=0.70\pm0.08\,\rm pc$. The cluster density profile merges into the background at a limiting radius $\mbox{$R_{\rm lim}$ }=6.5\pm0.5\,\rm pc$. From the field-star subtracted luminosity functions we derive the mass functions (MFs) in the form $\phi(m)\propto m^{-(1+\chi)}$. In the halo and through the whole cluster the MFs have slopes $\rm\chi=1.52\pm0.13$ and $\rm\chi=1.45\pm0.12$, respectively, thus slightly steeper than Salpeter's IMF. In the core the MF is flat, $\rm\chi=0.62\pm0.16$, 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 NGC 6611, part of this effect appears to be related to the molecular cloud-fragmentation process itself. We detect $362\pm120$ PMS stars. The total observed mass including detected MS (in the range $5{-}85\,\mbox{$M_\odot$ }$) and PMS stars amounts to ~ $1600\,\mbox{$M_\odot$ }$, 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.

Key words: Galaxy: open clusters and associations: individual: NGC 6611 -- Galaxy: structure

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© ESO 2005

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