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Astrophysical properties of binary star clusters in the Small Magellanic Cloud†

Published online by Cambridge University Press:  18 January 2010

João F. C. Santos Jr. ,
Alex A. Schmidt  and
Eduardo Bica
João F. C. Santos Jr.
Affiliation:
Departamento de Física, ICEx, Universidade Federal de Minas Gerais, Av. Antônio Carlos 6627, Belo Horizonte 31270-901, MG, Brazil email: jsantos@fisica.ufmg.br
Alex A. Schmidt
Affiliation:
Departamento de Matemática, Universidade Federal de Santa Maria, Av. Roraima 1000, Santa Maria 97105-900, RS, Brazil
Eduardo Bica
Affiliation:
Departamento de Astronomia, Universidade Federal do Rio Grande do Sul, Av. Bento Gonçalves 9500, Porto Alegre 91501-970, RS, Brazil
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Abstract

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To study the evolution of binary star clusters, we have imaged seven systems in the Small Magellanic Cloud with the SOAR 4m telescope using B and V filters. The sample contains pairs with well-separated components (d < 30 pc) as well as systems that apparently have merged, as evidenced by their unusual structures. By employing isochrone fitting to their color–magnitude diagrams, we have determined reddening values, ages and metallicities, and by fitting King models to their radial stellar-density profiles we estimated core radii. Disturbances of the density profiles are interpreted as evidence of interactions. Properties such as the distances between their components and their age differences are addressed in terms of the timescales involved, to assess the physical connection of the system. In two cases, the age difference is more than 50 Myr, which suggests a chance alignment, capture or sequential star formation.

Keywords

Magellanic Cloudsgalaxies: star clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S266: Star clusters: basic galactic building blocks throughout time and space , August 2009 , pp. 533 - 536
Copyright
Copyright © International Astronomical Union 2010

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