The VISCACHA survey - II. structure of star clusters in the magellanic clouds periphery

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dc.creatorJoão Francisco Coelho dos Santos Junior
dc.creatorAlexandre Roman Lopes
dc.creatorPieter Willem Westera
dc.creatorLuciano Fraga
dc.creatorBruno Corrêa Quint
dc.creatorDavid Sanmartim
dc.creatorFrancisco Ferreira de Souza Maia
dc.creatorBruno Moreira de Souza Dias
dc.creatorLeandro de Oliveira Kerber
dc.creatorAndrés Eduardo Piatti
dc.creatorEduardo Luiz Damiani Bica
dc.creatorMateus de Souza Angelo
dc.creatorDante Minniti del Barco
dc.creatorMaria de los Angeles Perez Villegas
dc.date.accessioned2024-02-20T15:32:43Z
dc.date.accessioned2025-09-09T00:54:47Z
dc.date.available2024-02-20T15:32:43Z
dc.date.issued2020
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico
dc.description.sponsorshipCAPES - Coordenação de Aperfeiçoamento de Pessoal de Nível Superior
dc.description.sponsorshipFAPESP - Fundação de Amparo à Pesquisa do Estado de São Paulo
dc.format.mimetypepdf
dc.identifier.doihttps://doi.org/10.1093/mnras/staa2425
dc.identifier.issn1365-2966
dc.identifier.urihttps://hdl.handle.net/1843/64310
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsAcesso Aberto
dc.subjectGaláxias
dc.subjectAglomerado de estrelas
dc.subject.otherGalaxies
dc.subject.otherMagellanic clouds
dc.subject.otherStar clusters
dc.titleThe VISCACHA survey - II. structure of star clusters in the magellanic clouds periphery
dc.typeArtigo de periódico
local.citation.epage222
local.citation.issue1
local.citation.spage205
local.citation.volume498
local.description.resumoWe 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.
local.identifier.orcidhttps://orcid.org/0000-0003-1794-6356
local.identifier.orcidhttps://orcid.org/0000-0002-1379-4204
local.identifier.orcidhttps://orcid.org/0000-0003-3379-994X
local.identifier.orcidhttps://orcid.org/0000-0003-0680-1979
local.identifier.orcidhttps://orcid.org/0000-0002-1557-3560
local.identifier.orcidhttps://orcid.org/0000-0002-9238-9521
local.identifier.orcidhttps://orcid.org/0000-0002-2569-4032
local.identifier.orcidhttps://orcid.org/0000-0003-4254-7111
local.identifier.orcidhttps://orcid.org/0000-0002-7435-8748
local.identifier.orcidhttps://orcid.org/0000-0002-8679-0589
local.identifier.orcidhttps://orcid.org/0000-0001-6138-0674
local.identifier.orcidhttps://orcid.org/0000-0002-7064-099X
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://academic.oup.com/mnras/article/498/1/205/5892585

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