Investigating dynamical properties of evolved Galactic open clusters
Autor(a) principal: | |
---|---|
Data de Publicação: | 2019 |
Outros Autores: | , , |
Tipo de documento: | Artigo |
Idioma: | por |
Título da fonte: | Repositório Institucional da UFMG |
Texto Completo: | https://doi.org/10.1051/0004-6361/201832702 http://hdl.handle.net/1843/51879 https://orcid.org/0000-0002-0246-3207 https://orcid.org/0000-0003-1794-6356 https://orcid.org/0000-0002-5150-5282 https://orcid.org/0000-0002-5166-8663 |
Resumo: | Context. 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. |
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2023-04-12T20:47:05Z2023-04-12T20:47:05Z2019624A8https://doi.org/10.1051/0004-6361/201832702http://hdl.handle.net/1843/51879https://orcid.org/0000-0002-0246-3207https://orcid.org/0000-0003-1794-6356https://orcid.org/0000-0002-5150-5282https://orcid.org/0000-0002-5166-8663Context. 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.porUniversidade Federal de Minas GeraisUFMGBrasilICX - DEPARTAMENTO DE FÍSICAA&AGalaxias - AglomeradosOpen clustersAssociations: generalInvestigating dynamical properties of evolved Galactic open clustersinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttps://www.aanda.org/articles/aa/full_html/2019/04/aa32702-18/aa32702-18.htmlMateus de Souza ÂngeloJoao F. C. Santos Jr.Wagner José Corradi BarbosaFrancisco Ferreira de Souza Maiainfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFMGinstname:Universidade Federal de Minas Gerais (UFMG)instacron:UFMGLICENSELicense.txtLicense.txttext/plain; charset=utf-82042https://repositorio.ufmg.br/bitstream/1843/51879/1/License.txtfa505098d172de0bc8864fc1287ffe22MD51ORIGINALInvestigating dynamical properties of evolved Galactic open clusters.pdfInvestigating dynamical properties of evolved Galactic open clusters.pdfapplication/pdf13235687https://repositorio.ufmg.br/bitstream/1843/51879/2/Investigating%20dynamical%20properties%20of%20evolved%20Galactic%20open%20clusters.pdf2354d424ca7f578d26e781f7b983664fMD521843/518792023-04-12 17:47:05.188oai:repositorio.ufmg.br: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Repositório de PublicaçõesPUBhttps://repositorio.ufmg.br/oaiopendoar:2023-04-12T20:47:05Repositório Institucional da UFMG - Universidade Federal de Minas Gerais (UFMG)false |
dc.title.pt_BR.fl_str_mv |
Investigating dynamical properties of evolved Galactic open clusters |
title |
Investigating dynamical properties of evolved Galactic open clusters |
spellingShingle |
Investigating dynamical properties of evolved Galactic open clusters Mateus de Souza Ângelo Open clusters Associations: general Galaxias - Aglomerados |
title_short |
Investigating dynamical properties of evolved Galactic open clusters |
title_full |
Investigating dynamical properties of evolved Galactic open clusters |
title_fullStr |
Investigating dynamical properties of evolved Galactic open clusters |
title_full_unstemmed |
Investigating dynamical properties of evolved Galactic open clusters |
title_sort |
Investigating dynamical properties of evolved Galactic open clusters |
author |
Mateus de Souza Ângelo |
author_facet |
Mateus de Souza Ângelo Joao F. C. Santos Jr. Wagner José Corradi Barbosa Francisco Ferreira de Souza Maia |
author_role |
author |
author2 |
Joao F. C. Santos Jr. Wagner José Corradi Barbosa Francisco Ferreira de Souza Maia |
author2_role |
author author author |
dc.contributor.author.fl_str_mv |
Mateus de Souza Ângelo Joao F. C. Santos Jr. Wagner José Corradi Barbosa Francisco Ferreira de Souza Maia |
dc.subject.por.fl_str_mv |
Open clusters Associations: general |
topic |
Open clusters Associations: general Galaxias - Aglomerados |
dc.subject.other.pt_BR.fl_str_mv |
Galaxias - Aglomerados |
description |
Context. 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. |
publishDate |
2019 |
dc.date.issued.fl_str_mv |
2019 |
dc.date.accessioned.fl_str_mv |
2023-04-12T20:47:05Z |
dc.date.available.fl_str_mv |
2023-04-12T20:47:05Z |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/1843/51879 |
dc.identifier.doi.pt_BR.fl_str_mv |
https://doi.org/10.1051/0004-6361/201832702 |
dc.identifier.orcid.pt_BR.fl_str_mv |
https://orcid.org/0000-0002-0246-3207 https://orcid.org/0000-0003-1794-6356 https://orcid.org/0000-0002-5150-5282 https://orcid.org/0000-0002-5166-8663 |
url |
https://doi.org/10.1051/0004-6361/201832702 http://hdl.handle.net/1843/51879 https://orcid.org/0000-0002-0246-3207 https://orcid.org/0000-0003-1794-6356 https://orcid.org/0000-0002-5150-5282 https://orcid.org/0000-0002-5166-8663 |
dc.language.iso.fl_str_mv |
por |
language |
por |
dc.relation.ispartof.pt_BR.fl_str_mv |
A&A |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.publisher.none.fl_str_mv |
Universidade Federal de Minas Gerais |
dc.publisher.initials.fl_str_mv |
UFMG |
dc.publisher.country.fl_str_mv |
Brasil |
dc.publisher.department.fl_str_mv |
ICX - DEPARTAMENTO DE FÍSICA |
publisher.none.fl_str_mv |
Universidade Federal de Minas Gerais |
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reponame:Repositório Institucional da UFMG instname:Universidade Federal de Minas Gerais (UFMG) instacron:UFMG |
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