Ages and metallicities of stellar clusters using S-PLUS narrow-band integrated photometry: the Small Magellanic Cloud

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dc.contributor.authorFabiano De Souza G.
dc.contributor.authorWestera P.
dc.contributor.authorAlmeida-Fernandes F.
dc.contributor.authorLimberg G.
dc.contributor.authorDias B.
dc.contributor.authorHernandez-Jimenez J.A.
dc.contributor.authorHerpich F.R.
dc.contributor.authorKerber L.O.
dc.contributor.authorMacHado-Pereira E.
dc.contributor.authorPerottoni H.D.
dc.contributor.authorGuerço, Rafael
dc.contributor.authorLi L.
dc.contributor.authorSampedro L.
dc.contributor.authorKanaan A.
dc.contributor.authorRibeiro T.
dc.contributor.authorSchoenell W.
dc.contributor.authorMendes De Oliveira C.
dc.date.accessioned2024-11-26T17:33:59Z
dc.date.available2024-11-26T17:33:59Z
dc.date.issued2024-01
dc.descriptionIndexación: Scopus
dc.description.abstractThe Magellanic Clouds are the most massive and closest satellite galaxies of the Milky Way (MW), with stars covering ages from a few Myr up to 13 Gyr. This makes them important for validating integrated light methods to study stellar populations and star formation processes, which can be applied to more distant galaxies. We characterized a set of stellar clusters in the Small Magellanic Cloud (SMC), using the Southern Photometric Local Universe Survey. This is the first age (metallicity) determination for 11 (65) clusters of this sample. Through its seven narrow bands, centred on important spectral features, and five broad bands, we can retrieve detailed information about stellar populations. We obtained ages and metallicities for all stellar clusters using the Bayesian spectral energy distribution fitting code bagpipes. With a sample of clusters in the colour range -0.20 < r - z < +0.35, for which our determined parameters are most reliable, we modeled the age-metallicity relation of SMC. At any given age, the metallicities of SMC clusters are lower than those of both the Gaia Sausage-Enceladus disrupted dwarf galaxy and the MW. In comparison with literature values, differences are Δlog(age) ≈ 0.31 and Δ[Fe/H] ≈ 0.41, which is comparable to low-resolution spectroscopy of individual stars. Finally, we confirm a previously known gradient, with younger clusters in the centre and older ones preferentially located in the outermost regions. On the other hand, we found no evidence of a significant metallicity gradient. © 2023 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.
dc.description.urihttps://academic-oup-com.recursosbiblioteca.unab.cl/mnras/article/527/2/1733/7330786?login=true&token=eyJhbGciOiJub25lIn0.eyJleHAiOjE3MzUyMzM0NTAsImp0aSI6IjQ3YjA1Y2M3LWYzNDctNDlhOS1iMGIzLWNiOGRlZWFjOTg3ZCJ9.
dc.identifier.citationMonthly Notices of the Royal Astronomical Society. Volume 527, Issue 2, Pages 1733 - 1744. 1 January 2024
dc.identifier.doi10.1093/mnras/stad3276
dc.identifier.issn0035-8711
dc.identifier.urihttps://repositorio.unab.cl/handle/ria/62260
dc.language.isoen
dc.publisherOxford University Press
dc.rights.licenseAttribution-NonCommercial-NoDerivatives 4.0 International Deed ( CC BY-NC-ND 4.0)
dc.rights.licensehttps://creativecommons.org/licenses/by-nc-nd/4.0/
dc.subjectGalaxies: Photometry
dc.subjectGalaxies: Star Clusters: General
dc.subjectMagellanic Clouds
dc.titleAges and metallicities of stellar clusters using S-PLUS narrow-band integrated photometry: the Small Magellanic Cloud
dc.typeArtículo
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