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The seven sisters DANCe

hal.structure.identifierM2A 2018
dc.contributor.authorOLIVARES, J.
dc.contributor.authorMORAUX, E.
dc.contributor.authorSARRO, L. M.
hal.structure.identifierM2A 2018
dc.contributor.authorBOUY, H.
dc.contributor.authorBERIHUETE, A.
dc.contributor.authorBARRADO, D.
dc.contributor.authorHUELAMO, N.
dc.contributor.authorBERTIN, E.
dc.contributor.authorBOUVIER, J.
dc.date.accessioned2021-07-07T15:54:26Z
dc.date.available2021-07-07T15:54:26Z
dc.date.issued2018-04
dc.identifier.issn0004-6361
dc.identifier.urihttps://oskar-bordeaux.fr/handle/20.500.12278/95445
dc.description.abstractEnContext. Membership analyses of the DANCe and Tycho + DANCe data sets provide the largest and least contaminated sample of Pleiades candidate members to date. Aims: We aim at reassessing the different proposals for the number surface density of the Pleiades in the light of the new and most complete list of candidate members, and inferring the parameters of the most adequate model. Methods: We compute the Bayesian evidence and Bayes Factors for variations of the classical radial models. These include elliptical symmetry, and luminosity segregation. As a by-product of the model comparison, we obtain posterior distributions for each set of model parameters. Results: We find that the model comparison results depend on the spatial extent of the region used for the analysis. For a circle of 11.5 parsecs around the cluster centre (the most homogeneous and complete region), we find no compelling reason to abandon King's model, although the Generalised King model introduced here has slightly better fitting properties. Furthermore, we find strong evidence against radially symmetric models when compared to the elliptic extensions. Finally, we find that including mass segregation in the form of luminosity segregation in the J band is strongly supported in all our models. Conclusions: We have put the question of the projected spatial distribution of the Pleiades cluster on a solid probabilistic framework, and inferred its properties using the most exhaustive and least contaminated list of Pleiades candidate members available to date. Our results suggest however that this sample may still lack about 20% of the expected number of cluster members. Therefore, this study should be revised when the completeness and homogeneity of the data can be extended beyond the 11.5 parsecs limit. Such a study will allow for more precise determination of the Pleiades spatial distribution, its tidal radius, ellipticity, number of objects and total mass.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enastrometry
dc.subject.enopen clusters and associations: individual: M 45
dc.subject.eninfrared: stars
dc.subject.enmethods: data analysis
dc.subject.enmethods: statistical
dc.title.enThe seven sisters DANCe
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201731996
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Instrumentation et méthodes pour l'astrophysique [astro-ph.IM]
dc.identifier.arxiv1711.11037
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA70
bordeaux.volume612
bordeaux.hal.laboratoriesLaboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804*
bordeaux.institutionCNRS
bordeaux.institutionUniversité de Bordeaux
bordeaux.peerReviewedoui
hal.identifierhal-01982370
hal.version1
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01982370v1
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