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dc.contributor.author
Parisi, Maria Celeste
dc.contributor.author
Geisler, Doug
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Carraro, G.
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Claria Olmedo, Juan Jose
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Costa, E
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Grocholski, A.J.
dc.contributor.author
Sarajedini, A.
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Leiton, R.
dc.contributor.author
Piatti, Andres Eduardo
dc.date.available
2018-01-18T14:14:33Z
dc.date.issued
2014-01
dc.identifier.citation
Parisi, Maria Celeste; Geisler, Doug; Carraro, G.; Claria Olmedo, Juan Jose; Costa, E; et al.; Age Determination of 15 Old to Intermediate-Age Small Magellanic Cloud Star Clusters; IOP Publishing; Astronomical Journal; 147; 71; 1-2014; 71-88
dc.identifier.issn
0004-6256
dc.identifier.uri
http://hdl.handle.net/11336/33753
dc.description.abstract
We present color–magnitude diagrams in theVandIbands for 15 star clusters in the Small Magellanic Cloud (SMC)based on data taken with the Very Large Telescope (VLT, Chile). We selected these clusters from our previouswork, wherein we derived cluster radial velocities and metallicities from calcium II infrared triplet (CaT) spectraalso taken with the VLT. We discovered that the ages of six of our clusters have been appreciably underestimatedby previous studies, which used comparatively small telescopes, graphically illustrating the need for large aperturesto obtain reliable ages of old and intermediate-age SMC star clusters. In particular, three of these clusters, L4, L6,and L110, turn out to be among the oldest SMC clusters known, with ages of 7.9±1.1, 8.7±1.2, and 7.6±1.0 Gyr, respectively, helping to fill a possible “SMC cluster age gap.” Using the current ages and metallicities fromParisi et al., we analyze the age distribution, age gradient, and age–metallicity relation (AMR) of a sample of SMCclusters measured homogeneously. There is a suggestion of bimodality in the age distribution but it does not showa constant slope for the first 4 Gyr, and we find no evidence for an age gradient. Due to the improved ages of ourcluster sample, we find that our AMR is now better represented in the intermediate/old period than we had derivedin Parisi et al., where we simply took ages available in the literature. Additionally, clusters younger than∼4Gyrnow show better agreement with the bursting model of Pagel & Tautvaiˇsien ̇e, but we confirm that this model isnot a good representation of the AMR during the intermediate/old period. A more complicated model is needed toexplain the SMC chemical evolution in that period.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
IOP Publishing
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Galaxies: Star
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Clusters: General
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Magellanic Cloudsonline
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Only Material:Color Figures
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Extended Figure
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Astronomía
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Ciencias Físicas
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CIENCIAS NATURALES Y EXACTAS
dc.title
Age Determination of 15 Old to Intermediate-Age Small Magellanic Cloud Star Clusters
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2018-01-17T15:03:41Z
dc.journal.volume
147
dc.journal.number
71
dc.journal.pagination
71-88
dc.journal.pais
Estados Unidos
dc.journal.ciudad
Madison
dc.description.fil
Fil: Parisi, Maria Celeste. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba; Argentina
dc.description.fil
Fil: Geisler, Doug. Universidad de Concepción; Chile
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Fil: Carraro, G.. European Southern Observatory. Santiago de Chile; Chile
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Fil: Claria Olmedo, Juan Jose. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba; Argentina
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Fil: Costa, E. Universidad de Chile; Chile
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Fil: Grocholski, A.J.. State University of Louisiana; Estados Unidos
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Fil: Sarajedini, A.. University of Florida; Estados Unidos
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Fil: Leiton, R.. Universidad de Concepción; Chile
dc.description.fil
Fil: Piatti, Andres Eduardo. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba; Argentina
dc.journal.title
Astronomical Journal
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1088/0004-6256/147/4/71
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-6256/147/4/71/meta
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