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dc.contributor.authorSaroon, Sasipt_BR
dc.contributor.authorDias, Brunopt_BR
dc.contributor.authorTsujimoto, Takujipt_BR
dc.contributor.authorParisi, M. C.pt_BR
dc.contributor.authorMaia, Francisco F. S.pt_BR
dc.contributor.authorKerber, Leandro de Oliveirapt_BR
dc.contributor.authorBekki, Kenjipt_BR
dc.contributor.authorMinniti, Dantept_BR
dc.contributor.authorOliveira, Raphael Augusto Pereira dept_BR
dc.contributor.authorWestera, Pieterpt_BR
dc.contributor.authorSantrich, Orlando J. Katimept_BR
dc.contributor.authorBica, Eduardo Luiz Damianipt_BR
dc.contributor.authorSanmartim, Davidpt_BR
dc.contributor.authorQuint, Bruno C.pt_BR
dc.contributor.authorFraga, Lucianopt_BR
dc.date.accessioned2024-01-13T03:42:38Zpt_BR
dc.date.issued2023pt_BR
dc.identifier.issn0004-6361pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/270986pt_BR
dc.description.abstractThe chemical evolution history of the Small Magellanic Cloud (SMC) has been a matter of debate for decades. The challenges in understanding the SMC chemical evolution are related to a very slow star formation rate (SFR) combined with bursts triggered by the multiple interactions between the SMC and the Large Magellanic Cloud, a significant (∼0.5 dex) metallicity dispersion for the SMC cluster population younger than about 7.5 Gyr, and multiple chemical evolution models tracing very different paths through the observed age–metallicity relation of the SMC. There is no doubt that these processes were complex. Therefore, a step-by-step strategy is required in order to better understand the SMC chemical evolution. We adopted an existing framework to split the SMC into regions on the sky, and we focus on the west halo in this work, which contains the oldest and most metal-poor stellar populations and is moving away from the SMC, that is, in an opposite motion with respect to the Magellanic Bridge. We present a sample containing ∼60% of all west halo clusters to represent the region well, and we identify a clear age–metallicity relation with a tight dispersion that exhibits a 0.5 dex metallicity dip about 6 Gyr ago. We ran chemical evolution models and discuss possible scenarios to explain this metallicity dip, the most likely being a major merger accelerating the SFR after the event. This merger should be combined with inefficient internal gas mixing within the SMC and different SFRs in different SMC regions because the same metallicity dip is not seen in the AMR of the SMC combining clusters from all regions. We try to explain the scenario to better understand the SMC chemo-dynamical history.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofAstronomy and astrophysics. Les Ulis. Vol. 677 (Sept. 2023), A35, 16 p.pt_BR
dc.rightsOpen Accessen
dc.subjectGaláxias anãspt_BR
dc.subjectGalaxies: dwarfen
dc.subjectNuvens de magalhaespt_BR
dc.subjectGalaxies: interactionsen
dc.subjectMagellanic Cloudsen
dc.subjectAglomerados de galaxiaspt_BR
dc.subjectGalaxies: clusters: generalen
dc.titleThe VISCACHA survey : VIII. Chemical evolution history of the small Magellanic cloud west halo clusterspt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb001194110pt_BR
dc.type.originEstrangeiropt_BR


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