Washington photometry of candidate star clusters in the Small Magellanic Cloud

We present for the first time Washington CT1 photometry for 11 unstudied or poorly studied candidate star clusters. The selected objects are of small angular size, contain a handful of stars, and are projected towards the innermost regions of the Small Magellanic Cloud (SMC). The respective colour-m...

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Guardado en:
Detalles Bibliográficos
Publicado: 2012
Materias:
General
Individual
Photometric - galaxies
SMC - galaxies
Star clusters
Techniques
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v425_n4_p3085_Piatti
http://hdl.handle.net/20.500.12110/paper_00358711_v425_n4_p3085_Piatti
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00358711_v425_n4_p3085_Piatti
record_format dspace
spelling paper:paper_00358711_v425_n4_p3085_Piatti2023-06-08T15:01:34Z Washington photometry of candidate star clusters in the Small Magellanic Cloud General Individual Photometric - galaxies SMC - galaxies Star clusters Techniques We present for the first time Washington CT1 photometry for 11 unstudied or poorly studied candidate star clusters. The selected objects are of small angular size, contain a handful of stars, and are projected towards the innermost regions of the Small Magellanic Cloud (SMC). The respective colour-magnitude diagrams (CMDs) were cleaned of the unavoidable star field contamination by taking advantage of a procedure which makes use of variable size CMD cells. This method has shown to be able to eliminate stochastic effects in the cluster CMDs caused by the presence of isolated bright stars, as well as to make a finer cleaning in the most populous CMD regions. Our results suggest that nearly one-third of the studied candidate star clusters would appear to be genuine physical systems. In this sense, the ages previously derived for some of them mostly reflect those of the composite stellar populations of the SMC field. Finally, we used the spatial distribution in the SMC of possible non-clusters to statistically decontaminate that of the SMC cluster system. We found that there is no clear difference between expected and observed cluster spatial distributions, although it would become significant at a 2σ level between a ≈ 0°. 3 and 1°. 2 (the semi-major axis of an ellipse parallel to the SMC bar and with b/a = 1/2), if the asterisms were increased up to 20 per cent. © 2012 The Authors. 2012 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v425_n4_p3085_Piatti http://hdl.handle.net/20.500.12110/paper_00358711_v425_n4_p3085_Piatti
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic General
Individual
Photometric - galaxies
SMC - galaxies
Star clusters
Techniques
spellingShingle General
Individual
Photometric - galaxies
SMC - galaxies
Star clusters
Techniques
Washington photometry of candidate star clusters in the Small Magellanic Cloud
topic_facet General
Individual
Photometric - galaxies
SMC - galaxies
Star clusters
Techniques
description We present for the first time Washington CT1 photometry for 11 unstudied or poorly studied candidate star clusters. The selected objects are of small angular size, contain a handful of stars, and are projected towards the innermost regions of the Small Magellanic Cloud (SMC). The respective colour-magnitude diagrams (CMDs) were cleaned of the unavoidable star field contamination by taking advantage of a procedure which makes use of variable size CMD cells. This method has shown to be able to eliminate stochastic effects in the cluster CMDs caused by the presence of isolated bright stars, as well as to make a finer cleaning in the most populous CMD regions. Our results suggest that nearly one-third of the studied candidate star clusters would appear to be genuine physical systems. In this sense, the ages previously derived for some of them mostly reflect those of the composite stellar populations of the SMC field. Finally, we used the spatial distribution in the SMC of possible non-clusters to statistically decontaminate that of the SMC cluster system. We found that there is no clear difference between expected and observed cluster spatial distributions, although it would become significant at a 2σ level between a ≈ 0°. 3 and 1°. 2 (the semi-major axis of an ellipse parallel to the SMC bar and with b/a = 1/2), if the asterisms were increased up to 20 per cent. © 2012 The Authors.
title Washington photometry of candidate star clusters in the Small Magellanic Cloud
title_short Washington photometry of candidate star clusters in the Small Magellanic Cloud
title_full Washington photometry of candidate star clusters in the Small Magellanic Cloud
title_fullStr Washington photometry of candidate star clusters in the Small Magellanic Cloud
title_full_unstemmed Washington photometry of candidate star clusters in the Small Magellanic Cloud
title_sort washington photometry of candidate star clusters in the small magellanic cloud
publishDate 2012
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v425_n4_p3085_Piatti
http://hdl.handle.net/20.500.12110/paper_00358711_v425_n4_p3085_Piatti
_version_ 1768541648050978816

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