The VISCACHA survey - V. Rejuvenating three faint SMC clusters

dc.creatorEduardo Luiz Damiani Bica
dc.creatorMaría Celeste Parisi
dc.creatorStefano Oliveira de Souza
dc.creatorBeatriz Leonor Silveira Barbuy
dc.creatorFrancisco Ferreira de Souza Maia
dc.creatorRaphael Augusto Pereira de Oliveira
dc.creatorBruno Moreira de Souza Dias
dc.creatorJoão Francisco Coelho dos Santos Junior
dc.creatorJoão Pedro Rocha
dc.creatorLeandro de Oliveira Kerber
dc.creatorJoão Francisco Gardin de Carvalho
dc.creatorAna Cristina Moreira Machado Zadra Armond
dc.date.accessioned2024-02-20T16:43:48Z
dc.date.accessioned2025-09-08T23:37:20Z
dc.date.available2024-02-20T16:43:48Z
dc.date.issued2022
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico
dc.description.sponsorshipCAPES - Coordenação de Aperfeiçoamento de Pessoal de Nível Superior
dc.description.sponsorshipFAPERJ - Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
dc.description.sponsorshipFAPESP - Fundação de Amparo à Pesquisa do Estado de São Paulo
dc.format.mimetypepdf
dc.identifier.doihttps://doi.org/10.1093/mnrasl/slac108
dc.identifier.issn1745-3933
dc.identifier.urihttps://hdl.handle.net/1843/64328
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society: Letters
dc.rightsAcesso Aberto
dc.subjectAglomerado de estrelas
dc.subject.otherMagellanic clouds
dc.subject.otherStar clusters
dc.titleThe VISCACHA survey - V. Rejuvenating three faint SMC clusters
dc.typeArtigo de periódico
local.citation.epageL45
local.citation.issue1
local.citation.spageL41
local.citation.volume517
local.description.resumoWe present the analysis of three faint clusters of the Small Magellanic Cloud RZ 82, HW 42, and RZ 158. We employed the SOAR telescope instrument SAM with adaptive optics, allowing us to reach to V ∼ 23–24 mag, unprecedentedly, a depth sufficient to measure ages of up to about 10–12 Gyr. All three clusters are resolved to their centres, and the resulting colour–magnitude diagrams (CMDs) allow us to derive ages of 3.9, 2.6, and 4.8 Gyr, respectively. These results are significantly younger than previous determinations (7.1, 5.0, and 8.3 Gyr, respectively), based on integrated photometry or shallower CMDs. We rule out older ages for these clusters based on deep photometry and statistical isochrone fitting. We also estimate metallicities for the three clusters of [Fe/H] = −0.68, −0.57, and −0.90, respectively. These updated ages and metallicities are in good agreement with the age-metallicity relation for the bulk of SMC clusters. Total cluster masses ranging from ∼ 7–11 · 103 M were estimated from integrated flux, consistent with masses estimated for other SMC clusters of similar ages. These results reduce the number of SMC clusters known to be older than about 5 Gyr and highlight the need of deep and spatially resolved photometry to determine accurate ages for older low-luminosity SMC star clusters.
local.identifier.orcidhttps://orcid.org/0000-0001-9382-3986
local.identifier.orcidhttps://orcid.org/0000-0001-8052-969X
local.identifier.orcidhttps://orcid.org/0000-0001-9264-4417
local.identifier.orcidhttps://orcid.org/0000-0002-2569-4032
local.identifier.orcidhttps://orcid.org/0000-0002-4778-9243
local.identifier.orcidhttps://orcid.org/0000-0003-4254-7111
local.identifier.orcidhttps://orcid.org/0000-0003-1794-6356
local.identifier.orcidhttps://orcid.org/0000-0001-7561-5067
local.identifier.orcidhttps://orcid.org/0000-0002-7435-8748
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://academic.oup.com/mnrasl/article/517/1/L41/6701629

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