Open clusters in the Third Galactic Quadrant : III. Alleged binary clusters

Aims: We aim to determine accurate distances and ages of eight open clusters in order to: (1) assess their possible binarity (2) provide probes to trace the structure of the Third Galactic Quadrant. Methods: Cluster reddenings, distances, ages and metallicities are derived from ZAMS and isochrone fi...

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Detalles Bibliográficos
Autores principales: Vázquez, Rubén Ángel, Moitinho, A., Carraro, G., Dias, W. S.
Formato: Articulo
Lenguaje:Inglés
Publicado: 2010
Materias:
Ciencias Astronómicas
Galaxy: structure
Open clusters and associations: general
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/82627
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-82627
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
Galaxy: structure
Open clusters and associations: general
spellingShingle Ciencias Astronómicas
Galaxy: structure
Open clusters and associations: general
Vázquez, Rubén Ángel
Moitinho, A.
Carraro, G.
Dias, W. S.
Open clusters in the Third Galactic Quadrant : III. Alleged binary clusters
topic_facet Ciencias Astronómicas
Galaxy: structure
Open clusters and associations: general
description Aims: We aim to determine accurate distances and ages of eight open clusters in order to: (1) assess their possible binarity (2) provide probes to trace the structure of the Third Galactic Quadrant. Methods: Cluster reddenings, distances, ages and metallicities are derived from ZAMS and isochrone fits in UBVRI photometric diagrams. Field contamination is reduced by restricting analysis to stars within the cluster limits derived from star counts. Further membership control is done by requiring that stars have consistent positions in several diagrams and by using published spectral types. Results: The derived distances, ages and metallicities have shown that none of the analysed clusters compose binary/double systems. Of the four candidate pairs, only NGC 2383/NGC 2384 are close to each other, but have different metallicities and ages. Ruprecht 72 and Ruprecht 158 are not clusters but fluctuations of the field stellar density. Haffner 18 is found to be the superposition of two stellar groups at different distances: Haffner 18(1) at 4.5 kpc and Haffner 18(2) between 9.5 and 11.4 kpc from the Sun. The derived distances and ages have been used to situate the clusters in the Galactic context. In particular, young stellar groups trace spiral structure at large Galactocentric radii. At least two clusters formed during the last few 108 yr in an interstellar medium with less than solar abundances. Conclusions: In contrast with the LMC, double clusters are apparently rare, or even non existent, in the undisturbed environment of the Third Galactic Quadrant. This leaves open the question of whether binary clusters form more easily toward denser and more violent regions of the Milky Way such as the inner Galaxy.
format Articulo
Articulo
author Vázquez, Rubén Ángel
Moitinho, A.
Carraro, G.
Dias, W. S.
author_facet Vázquez, Rubén Ángel
Moitinho, A.
Carraro, G.
Dias, W. S.
author_sort Vázquez, Rubén Ángel
title Open clusters in the Third Galactic Quadrant : III. Alleged binary clusters
title_short Open clusters in the Third Galactic Quadrant : III. Alleged binary clusters
title_full Open clusters in the Third Galactic Quadrant : III. Alleged binary clusters
title_fullStr Open clusters in the Third Galactic Quadrant : III. Alleged binary clusters
title_full_unstemmed Open clusters in the Third Galactic Quadrant : III. Alleged binary clusters
title_sort open clusters in the third galactic quadrant : iii. alleged binary clusters
publishDate 2010
url http://sedici.unlp.edu.ar/handle/10915/82627
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AT moitinhoa openclustersinthethirdgalacticquadrantiiiallegedbinaryclusters
AT carrarog openclustersinthethirdgalacticquadrantiiiallegedbinaryclusters
AT diasws openclustersinthethirdgalacticquadrantiiiallegedbinaryclusters
bdutipo_str Repositorios
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