Seven young star clusters in the inner region of the Small Magellanic Cloud

We present CCD photometry in the Washington system C and T 1 passbands down to T 1 ∼ 22 in the fields of L35, L45, L49, L50, L62, L63 and L85, seven poorly studied star clusters in the inner region of the Small Magellanic Cloud (SMC). We measured T 1 magnitudes and C - T 1 colours for a total of 114...

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Guardado en:
Detalles Bibliográficos
Publicado: 2008
Materias:
Galaxies: individual: SMC
Galaxies: star clusters
Magellanic Clouds
Techniques: photometric
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v389_n1_p429_Piatti
http://hdl.handle.net/20.500.12110/paper_00358711_v389_n1_p429_Piatti
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00358711_v389_n1_p429_Piatti
record_format dspace
spelling paper:paper_00358711_v389_n1_p429_Piatti2023-06-08T15:01:24Z Seven young star clusters in the inner region of the Small Magellanic Cloud Galaxies: individual: SMC Galaxies: star clusters Magellanic Clouds Techniques: photometric We present CCD photometry in the Washington system C and T 1 passbands down to T 1 ∼ 22 in the fields of L35, L45, L49, L50, L62, L63 and L85, seven poorly studied star clusters in the inner region of the Small Magellanic Cloud (SMC). We measured T 1 magnitudes and C - T 1 colours for a total of 114 826 stars distributed throughout cluster areas of 13.7 × 13.7 arcmin 2 each. Cluster radii were estimated from star counts distributed throughout the entire observed fields. The seven clusters are generally characterized by a relatively small angular size and by a high field star contamination. We performed an in-depth analysis of the field star contamination of the colour-magnitude diagrams (CMDs), and statistically cleaned the cluster CMDs. Based on the best fits of isochrones computed by the Padova group to the (T 1, C - T 1) CMDs, we derive ages for the sample, assuming Z = 0.004, finding ages between 25 Myr and 1.2 Gyr. We then examined different relationships between positions in the SMC, age and metallicity of a larger sample of clusters including our previous work whose ages and metallicities are on the same scale used in this paper. We confirm previous results in the sense that the further a cluster is from the centre of the galaxy, the older and more metal poor it is, with some dispersion; although clusters associated with the Magellanic Bridge clearly do not obey the general trend. The number of clusters within ∼ 2°of the SMC centre appears to have increased substantially after ∼2.5 Gyr ago, hinting at a burst. © 2008 RAS. 2008 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v389_n1_p429_Piatti http://hdl.handle.net/20.500.12110/paper_00358711_v389_n1_p429_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 Galaxies: individual: SMC
Galaxies: star clusters
Magellanic Clouds
Techniques: photometric
spellingShingle Galaxies: individual: SMC
Galaxies: star clusters
Magellanic Clouds
Techniques: photometric
Seven young star clusters in the inner region of the Small Magellanic Cloud
topic_facet Galaxies: individual: SMC
Galaxies: star clusters
Magellanic Clouds
Techniques: photometric
description We present CCD photometry in the Washington system C and T 1 passbands down to T 1 ∼ 22 in the fields of L35, L45, L49, L50, L62, L63 and L85, seven poorly studied star clusters in the inner region of the Small Magellanic Cloud (SMC). We measured T 1 magnitudes and C - T 1 colours for a total of 114 826 stars distributed throughout cluster areas of 13.7 × 13.7 arcmin 2 each. Cluster radii were estimated from star counts distributed throughout the entire observed fields. The seven clusters are generally characterized by a relatively small angular size and by a high field star contamination. We performed an in-depth analysis of the field star contamination of the colour-magnitude diagrams (CMDs), and statistically cleaned the cluster CMDs. Based on the best fits of isochrones computed by the Padova group to the (T 1, C - T 1) CMDs, we derive ages for the sample, assuming Z = 0.004, finding ages between 25 Myr and 1.2 Gyr. We then examined different relationships between positions in the SMC, age and metallicity of a larger sample of clusters including our previous work whose ages and metallicities are on the same scale used in this paper. We confirm previous results in the sense that the further a cluster is from the centre of the galaxy, the older and more metal poor it is, with some dispersion; although clusters associated with the Magellanic Bridge clearly do not obey the general trend. The number of clusters within ∼ 2°of the SMC centre appears to have increased substantially after ∼2.5 Gyr ago, hinting at a burst. © 2008 RAS.
title Seven young star clusters in the inner region of the Small Magellanic Cloud
title_short Seven young star clusters in the inner region of the Small Magellanic Cloud
title_full Seven young star clusters in the inner region of the Small Magellanic Cloud
title_fullStr Seven young star clusters in the inner region of the Small Magellanic Cloud
title_full_unstemmed Seven young star clusters in the inner region of the Small Magellanic Cloud
title_sort seven young star clusters in the inner region of the small magellanic cloud
publishDate 2008
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v389_n1_p429_Piatti
http://hdl.handle.net/20.500.12110/paper_00358711_v389_n1_p429_Piatti
_version_ 1768543268617846784

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