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Pre-main-sequence stars in the stellar association N 11 in the Large Magellanic Cloud: clustering properties

Published online by Cambridge University Press:  18 January 2010

Antonella Vallenari ,
Rosanna Sordo  and
Emanuela Chiosi
Antonella Vallenari
Affiliation:
INAF, Padova Observatory, Vicolo Osservatorio 5, 35122 Padova, Italy email: antonella.vallenari@oapd.inaf.it
Rosanna Sordo
Affiliation:
INAF, Padova Observatory, Vicolo Osservatorio 5, 35122 Padova, Italy email: antonella.vallenari@oapd.inaf.it
Emanuela Chiosi
Affiliation:
INAF, Padova Observatory, Vicolo Osservatorio 5, 35122 Padova, Italy email: antonella.vallenari@oapd.inaf.it
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Abstract

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Magellanic Clouds are of extreme importance to study the star-formation process in low-metallicity environments. Here, we discuss the clustering properties of the pre-main-sequence candidates and young embedded stellar objects in N 11, located in the Large Magellanic Cloud. Deep archival HST/ACS photometry is used to derive color–magnitude diagrams of the associations in N 11 and of the foreground field population. These data are complemented by archival infrared Spitzer data which allow detection of young embedded stellar objects. The spatial distribution of the pre-main-sequence candidates and young embedded stellar objects is discussed. The degree of clustering is derived using the minimal-spanning-tree method. No significant difference is found in clustering degree of young blue main-sequence stars and faint pre-main-sequence candidates, suggesting that they might be part of the same formation process.

Keywords

Magellanic Cloudsstars: pre–main-sequencestars: formation
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. 545 - 548
Copyright
Copyright © International Astronomical Union 2010

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