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dc.contributor.authorParisi, M. C.pt_BR
dc.contributor.authorOliveira, Raphael Augusto Pereira dept_BR
dc.contributor.authorAngelo, Mateus S.pt_BR
dc.contributor.authorDias, Bruno Moreira de Souzapt_BR
dc.contributor.authorMaia, Francisco F. S.pt_BR
dc.contributor.authorSaroon, Sasipt_BR
dc.contributor.authorFeinstein Baigorri, Carlospt_BR
dc.contributor.authorSantos Junior, Joao Francisco Coelho dospt_BR
dc.contributor.authorBica, Eduardo Luiz Damianipt_BR
dc.contributor.authorFerreira, Bernardo Pereira Limapt_BR
dc.contributor.authorFernández-Trincado, José Gregoriopt_BR
dc.contributor.authorWestera, Pieterpt_BR
dc.contributor.authorMinniti, Dantept_BR
dc.contributor.authorGarro, Elisa Ritapt_BR
dc.contributor.authorSantrich, Orlando J. Katimept_BR
dc.contributor.authorDe Bórtoli, Bruno Javierpt_BR
dc.contributor.authorSouza, Stefano O.pt_BR
dc.contributor.authorKerber, Leandro de Oliveirapt_BR
dc.contributor.authorPérez Villegas, Maria de Los Angelespt_BR
dc.date.accessioned2024-10-01T06:56:03Zpt_BR
dc.date.issued2024pt_BR
dc.identifier.issn0035-8711pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/279486pt_BR
dc.description.abstractThe structure of the Small Magellanic Cloud (SMC) outside of its main body is characterized by tidal branches resulting from its interactions mainly with the Large Magellanic Cloud (LMC). Characterizing the stellar populations in these tidal components helps to understand the dynamical history of this galaxy and of the Magellanic system in general. We provide full phase space vector information for Southern Bridge clusters. We performed a photometric and spectroscopic analysis of twelve SMC clusters, doubling the number of SMC clusters with full phase-space vector information known to date. We reclassify the sample considering 3D distances and 3D velocities. We found that some of the clusters classified as Southern Bridge objects according to the projected 2D classification actually belong to the Main Body and Counter-Bridge in the background. The comparison of the kinematics of the genuine foreground Bridge clusters with those previously analysed in the same way reveals that Southern Bridge clusters are moving towards the LMC and share the kinematics of the Northern Bridge. Adding to our sample clusters from the literature with CaT metallicity determinations we compare the age–metallicity relation of the Southern Bridge with the one of the Northern Bridge. We reinforce the idea that both regions do not seem to have experienced the same chemical enrichment history and that there is a clear absence of clusters in the Northern Bridge older than 3 Gyr and more metal poor than −1.1, which would not seem to be due to a selection effect.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofMonthly notices of the royal astronomical society. Oxford. Vol. 527, no. 4 (Feb. 2024), p. 10632–10648pt_BR
dc.rightsOpen Accessen
dc.subjectGalaxies : Evolutionen
dc.subjectEvolucao galaticapt_BR
dc.subjectNuvens de magalhaespt_BR
dc.subject(Galaxies) : Magellanic cloudsen
dc.subjectAglomerados estelarespt_BR
dc.subjectGalaxies : Star clusters : Generalen
dc.titleThe VISCACHA survey : IX. The SMC Southern Bridge in 8Dpt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb001201143pt_BR
dc.type.originEstrangeiropt_BR


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