The VISCACHA survey-II. Structure of star clusters in the Magellanic Clouds periphery

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dc.contributor.authorSantos, J.F.C.
dc.contributor.authorMaia, F.F.S.
dc.contributor.authorDias, B.
dc.contributor.authorKerber, L.D.O.
dc.contributor.authorPiatti, A.E.
dc.contributor.authorBica, E.
dc.contributor.authorAngelo, M.S.
dc.contributor.authorMinniti, D.
dc.contributor.authorPérez-Villegas, A.
dc.contributor.authorRoman-Lopes, A.
dc.contributor.authorWestera, P.
dc.contributor.authorFraga L.
dc.date.accessioned2021-10-26T13:01:24Z
dc.date.available2021-10-26T13:01:24Z
dc.date.issued2020-10
dc.descriptionIndexación: Scopus.es
dc.description.abstractWe provide a homogeneous set of structural parameters of 83 star clusters located at the periphery of the Small Magellanic Cloud (SMC) and the Large Magellanic Cloud (LMC). The clusters' stellar density and surface brightness profiles were built from deep, AO assisted optical images, and uniform analysis techniques. The structural parameters were obtained from King and Elson et al. model fittings. Integrated magnitudes and masses (for a subsample) are also provided. The sample contains mostly low surface brightness clusters with distances between 4.5 and 6.5 kpc and between 1 and 6.5 kpc from the LMC and SMC centres, respectively. We analysed their spatial distribution and structural properties, comparing them with those of inner clusters. Half-light and Jacobi radii were estimated, allowing an evaluation of the Roche volume tidal filling. We found that: (i) for our sample of LMC clusters, the tidal radii are, on average, larger than those of inner clusters from previous studies; (ii) the core radii dispersion tends to be greater for LMC clusters located towards the southwest, with position angles of ∼200° and about ∼5° from the LMC centre, i.e.Those LMC clusters nearer to the SMC; (iii) the core radius evolution for clusters with known age is similar to that of inner clusters; (iv) SMC clusters with galactocentric distances closer than 4 kpc are overfilling; (v) the recent Clouds collision did not leave marks on the LMC clusters' structure that our analysis could reveal. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.es
dc.description.urihttps://academic-oup-com.recursosbiblioteca.unab.cl/mnras/article/498/1/205/5892585
dc.identifier.citationMonthly Notices of the Royal Astronomical Society Open Access Volume 498, Issue 1, Pages 205 - 2221 October 2020es
dc.identifier.doi10.1093/mnras/staa2425
dc.identifier.issn0035-8711
dc.identifier.urihttp://repositorio.unab.cl/xmlui/handle/ria/20633
dc.language.isoenes
dc.publisherOxford University Presses
dc.subjectgalaxies: interactionses
dc.subjectgalaxies: photometryes
dc.subjectgalaxies: star clusters: generales
dc.subjectgalaxies:structurees
dc.subjectMagellanic Cloudses
dc.subjectsurveyses
dc.titleThe VISCACHA survey-II. Structure of star clusters in the Magellanic Clouds peripheryes
dc.typeArtículoes
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