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Please use this identifier to cite or link to this item: http://hdl.handle.net/1843/51879
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dc.creatorMateus de Souza Ângelopt_BR
dc.creatorJoao F. C. Santos Jr.pt_BR
dc.creatorWagner José Corradi Barbosapt_BR
dc.creatorFrancisco Ferreira de Souza Maiapt_BR
dc.date.accessioned2023-04-12T20:47:05Z-
dc.date.available2023-04-12T20:47:05Z-
dc.date.issued2019-
dc.citation.volume624pt_BR
dc.citation.spageA8pt_BR
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201832702pt_BR
dc.identifier.urihttp://hdl.handle.net/1843/51879-
dc.description.resumoContext. The stellar content of Galactic open clusters is gradually depleted during their evolution as a result of internal relaxation and external interactions. The final residues of the long-term evolution of open clusters are called open cluster remnants. These are sparsely populated structures that can barely be distinguished from the field. Aims.Weaimedtocharacteriseandcomparethedynamicalstatesofasetof16objectscataloguedasremnantsorremnantcandidates. We employed parameters that are intimately associated with the dynamical evolution: age, limiting radius, stellar mass, and velocity dispersion. The sample also includes 7 objects that are catalogued as dynamically evolved open clusters for comparison purposes. Methods. We used photometric data from the 2MASS catalogue, proper motions and parallaxes from the Gaia DR2 catalogue, and a decontamination algorithm that was applied to the three-dimensional astrometric space of proper motions and parallaxes (µα,µδ,$) forstarsintheobjects’areas.Theluminosityandmassfunctionsandtotalmassesformostopenclusterremnantsarederivedherefor the first time. Our analysis used predictions of N-body simulations to estimate the initial number of stars of the remnants from their dissolution timescales. Results. The investigated open cluster remnants present masses (M) and velocity dispersions (σv) within well-defined ranges: M between ∼10−40M and σv between ∼1−7kms−1. Some objects in the remnant sample have a limiting radius Rlim . 2pc, which meansthattheyaremorecompactthantheinvestigatedopenclusters;otherremnantshaveRlim between∼2−7pc,whichiscomparable to the open clusters. We suggest that cluster NGC2180 (previously classified as an open cluster) is entering a remnant evolutionary stage. In general, our clusters show signals of depletion of low-mass stars. This confirms their dynamically evolved states. Conclusions. We conclude that the open cluster remnants we studied are in fact remnants of initially very populous open clusters (N0 ∼ 103−104 stars). The outcome of the long-term evolution is to bring the final residues of the open clusters to dynamical states that are similar to each other, thus masking out the memory of the initial formation conditions of star clusters.pt_BR
dc.languageporpt_BR
dc.publisherUniversidade Federal de Minas Geraispt_BR
dc.publisher.countryBrasilpt_BR
dc.publisher.departmentICX - DEPARTAMENTO DE FÍSICApt_BR
dc.publisher.initialsUFMGpt_BR
dc.relation.ispartofA&Apt_BR
dc.rightsAcesso Abertopt_BR
dc.subjectOpen clusterspt_BR
dc.subjectAssociations: generalpt_BR
dc.subject.otherGalaxias - Aglomeradospt_BR
dc.titleInvestigating dynamical properties of evolved Galactic open clusterspt_BR
dc.typeArtigo de Periódicopt_BR
dc.url.externahttps://www.aanda.org/articles/aa/full_html/2019/04/aa32702-18/aa32702-18.htmlpt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-0246-3207pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-1794-6356pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-5150-5282pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-5166-8663pt_BR
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