NGC 6067: a young and massive open cluster with high metallicity

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Título: NGC 6067: a young and massive open cluster with high metallicity
Autor/es: Alonso-Santiago, Javier | Negueruela, Ignacio | Marco Tobarra, Amparo | Tabernero, Hugo M. | González-Fernández, Carlos | Castro, Norberto
Grupo/s de investigación o GITE: Astrofísica Estelar (AE)
Centro, Departamento o Servicio: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal
Palabras clave: Stars: abundances | Stars: fundamental parameters | Hertzsprung–Russell and colour–magnitude diagrams | Stars: late-type | Stars: variables: Cepheids | Open clusters and associations: individual: NGC 6067
Área/s de conocimiento: Astronomía y Astrofísica | Física Aplicada
Fecha de publicación: 30-mar-2017
Editor: Oxford University Press
Cita bibliográfica: Monthly Notices of the Royal Astronomical Society. 2017, 469(2): 1330-1353. doi:10.1093/mnras/stx783
Resumen: NGC 6067 is a young open cluster hosting the largest population of evolved stars among known Milky Way clusters in the 50–150 Ma age range. It thus represents the best laboratory in our Galaxy to constrain the evolutionary tracks of 5–7 M⊙ stars. We have used high-resolution spectra of a large sample of bright cluster members (45), combined with archival photometry, to obtain accurate parameters for the cluster as well as stellar atmospheric parameters. We derive a distance of 1.78 ± 0.12 kpc, an age of 90 ± 20 Ma and a tidal radius of 14.8 +6.8−3.2 arcmin. We estimate an initial mass above 5700 M⊙, for a present-day evolved population of two Cepheids, two A supergiants and 12 red giants with masses ≈6 M⊙. We also determine chemical abundances of Li, O, Na, Mg, Si, Ca, Ti, Ni, Rb, Y and Ba for the red clump stars. We find a supersolar metallicity, [Fe/H] = +0.19 ± 0.05, and a homogeneous chemical composition, consistent with the Galactic metallicity gradient. The presence of a Li-rich red giant, star 276 with A(Li) = 2.41, is also detected. An overabundance of Ba is found, supporting the enhanced s-process. The ratio of yellow to red giants is much smaller than 1, in agreement with models with moderate overshooting, but the properties of the cluster Cepheids do not seem consistent with current Padova models for supersolar metallicity.
Patrocinador/es: This research is partially supported by the Spanish Government Ministerio de Economía y Competitividad under grants BES 2013-065384 and AYA2015-68012-C2-2-P (MINECO/FEDER). AM acknowledges support from the Ministerio de Educación, Cultura y Deporte through grant PRX15/00030.
URI: http://hdl.handle.net/10045/68132
ISSN: 0035-8711 (Print) | 1365-2966 (Online)
DOI: 10.1093/mnras/stx783
Idioma: eng
Tipo: info:eu-repo/semantics/article
Derechos: © 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Revisión científica: si
Versión del editor: http://dx.doi.org/10.1093/mnras/stx783
Aparece en las colecciones:INV - Astrofísica Estelar - Artículos de Revistas

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