Characterizing dynamical states of Galactic open clusters with Gaia DR2

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dc.creatorMateus Angelo
dc.creatorWagner José Corradi Barbosa
dc.creatorJoao Francisco Coelho dos Santos Junior
dc.creatorFrancisco Maia
dc.creatorF. A. Ferreira
dc.date.accessioned2023-04-14T20:08:18Z
dc.date.accessioned2025-09-09T00:55:36Z
dc.date.available2023-04-14T20:08:18Z
dc.date.issued2021
dc.identifier.doihttps://doi.org/10.1093/mnras/staa3192
dc.identifier.issn00358711
dc.identifier.urihttps://hdl.handle.net/1843/51970
dc.languagepor
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsAcesso Restrito
dc.subjectGalaxias - Aglomerados
dc.subject.otherGalaxy: stellar content
dc.subject.otherOpen clusters and associations: general
dc.titleCharacterizing dynamical states of Galactic open clusters with Gaia DR2
dc.typeArtigo de periódico
local.citation.epage4353
local.citation.issue4
local.citation.spage4338
local.citation.volume500
local.description.resumoIn this work, we investigate the dynamical properties of 38 Galactic open clusters: 34 of them are located at low Galactic latitudes (|b| < 10°) and are projected against dense stellar fields; the other four comparison objects present clearer contrasts with the field population. We determine structural and time-related parameters that are associated with the clusters’ dynamical evolution: core (rc), tidal (rt), and half-mass (rhm) radii, ages (t), and crossing times (tcr). We have also incorporated results for 27 previously studied clusters, creating a sample of 65, spanning the age and Galactocentric distance (RG) ranges 7.0<logt<9.7 and 6 < RG (kpc) < 13. We employ a uniform analysis method which incorporates photometric and astrometric data from the Gaia DR2 catalogue. Member stars are identified by employing a decontamination algorithm which operates on the 3D astrometric space of parallax and proper motion and attributes membership likelihoods for stars in the cluster region. Our results show that internal relaxation causes rc to correlate negatively with the dynamical ratio τdyn = t/tcr. This implies that dynamically older systems tend to be more centrally concentrated. The more concentrated ones tend to present smaller rhm/rt ratios, which means that they are less subject to tidal disruption. The analysis of coeval groups at compatible RG suggests that the inner structure of clusters is reasonably insensitive to variations in the external tidal field. Additionally, our results confirm, on average, an increase in rt for regions with less-intense Galactic gravitational fields.
local.identifier.orcidhttps://orcid.org/0000-0001-6138-0674
local.identifier.orcidhttps://orcid.org/0000-0002-5150-5282
local.identifier.orcidhttps://orcid.org/0000-0001-9481-4547
local.identifier.orcidhttps://orcid.org/0000-0002-2569-4032
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://academic.oup.com/mnras/article/500/4/4338/6026637

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