Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12666/312
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dc.rights.license© ESO 2020-
dc.contributor.authorBaratella, M.-
dc.contributor.authorD´Orazi, V.-
dc.contributor.authorCarraro, G.-
dc.contributor.authorDesidera, S.-
dc.contributor.authorRandich, S.-
dc.contributor.authorMagrini, L.-
dc.contributor.authorAdibekyan, V.-
dc.contributor.authorSmiljanic, R.-
dc.contributor.authorSpina, L.-
dc.contributor.authorTsantaki, M.-
dc.contributor.authorTautvaisilenè, G.-
dc.contributor.authorSousa, S. G.-
dc.contributor.authorJofre, P.-
dc.contributor.authorJiménez Esteban, F. M.-
dc.contributor.authorDelgado Mena, E.-
dc.contributor.authorMartell, S.-
dc.contributor.authorVan der Swaelmen, M.-
dc.contributor.authorRoccatagliata, V.-
dc.contributor.authorGilmore, G.-
dc.contributor.authorAlfaro, Emilio J.-
dc.contributor.authorBayo, A.-
dc.contributor.authorBensby, T.-
dc.contributor.authorBragaglia, A.-
dc.contributor.authorFranciosini, E.-
dc.contributor.authorGonneau, A.-
dc.contributor.authorHeiter, U.-
dc.contributor.authorHourihane, A.-
dc.contributor.authorJeffries, R. D.-
dc.contributor.authorKoposov, S. E.-
dc.contributor.authorMorbidelli, L.-
dc.contributor.authorPrisinzano, L.-
dc.contributor.authorSacco, G.-
dc.contributor.authorSbordone, L.-
dc.contributor.authorWorley, Christopher-
dc.contributor.authorZaggia, S.-
dc.contributor.authorLewis, J.-
dc.contributor.otherUnidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737-
dc.date.accessioned2021-04-13T13:46:33Z-
dc.date.available2021-04-13T13:46:33Z-
dc.date.issued2020-01-31-
dc.identifier.citationAstronomy & Astrophysics 634: A34(2020)es
dc.identifier.issn0004-6361-
dc.identifier.otherhttps://www.aanda.org/articles/aa/full_html/2020/02/aa37055-19/aa37055-19.html-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/312-
dc.description.abstractContext. Open clusters are recognised as excellent tracers of Galactic thin-disc properties. At variance with intermediate-age and old open clusters, for which a significant number of studies is now available, clusters younger than ≲ 150 Myr have been mostly overlooked in terms of their chemical composition until recently (with few exceptions). On the other hand, previous investigations seem to indicate an anomalous behaviour of young clusters, which includes (but is not limited to) slightly sub-solar iron (Fe) abundances and extreme, unexpectedly high barium (Ba) enhancements. Aims. In a series of papers, we plan to expand our understanding of this topic and investigate whether these chemical peculiarities are instead related to abundance analysis techniques. Methods. We present a new determination of the atmospheric parameters for 23 dwarf stars observed by the Gaia-ESO survey in five young open clusters (τ < 150 Myr) and one star-forming region (NGC 2264). We exploit a new method based on titanium (Ti) lines to derive the spectroscopic surface gravity, and most importantly, the microturbulence parameter. A combination of Ti and Fe lines is used to obtain effective temperatures. We also infer the abundances of Fe » I, Fe » II, Ti » I, Ti » II, Na » I, Mg » I, Al » I, Si » I, Ca » I, Cr » I, and Ni » I. Results. Our findings are in fair agreement with Gaia-ESO iDR5 results for effective temperatures and surface gravities, but suggest that for very young stars, the microturbulence parameter is over-estimated when Fe lines are employed. This affects the derived chemical composition and causes the metal content of very young clusters to be under-estimated. Conclusions. Our clusters display a metallicity [Fe/H] between +0.04 ± 0.01 and +0.12 ± 0.02; they are not more metal poor than the Sun. Although based on a relatively small sample size, our explorative study suggests that we may not need to call for ad hoc explanations to reconcile the chemical composition of young open clusters with Galactic chemical evolution models. © ESO 2020.es
dc.description.sponsorshipWe thank the anonymous referee for very helpful comments and suggestions. This work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell' Istruzione, dell' Universita' e della Ricerca (MIUR) in the form of the grant "Premiale VLT 2012". The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. V.A. is supported by FCT -Fundacao para a Ciencia e a Tecnologia through national funds and by FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionalizacao by these grants: Investigador FCT contract nr. IF/00650/2015/CP1273/CT0001; UID/FIS/04434/2019; PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953 and PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113. F.J.E. acknowledges financial support from the Spanish MINECO/FEDER through grant AyA2017-84089. T.B. was supported by the project grant "The New Milky Way" from the Knut and Alice Wallenberg Foundation. U.H. acknowledges support from the Swedish National Space Agency (SNSA/Rymdstyrelsen). S.G.S acknowledges the support by Fundacao para a Ciencia e Tecnologia (FCT) through national funds and a research grant (project ref. UID/FIS/04434/2013, and PTDC/FIS-AST/7073/2014). S.G.S. also acknowledge the support from FCT through Investigador FCT contract of reference IF/00028/2014 and POPH/FSE (EC) by FEDER funding through the program -Programa Operacional de Factores de Competitividade -COMPETE; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).es
dc.language.isoenges
dc.publisherEDP Scienceses
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2017-84089-P/ES/EL OBSERVATORIO VIRTUAL ESPAÑOL. EXPLOTACION CIENTIFICO-TECNICA DE ARCHIVOS ASTRONOMICOS/-
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/4.0/*
dc.subjectOpen clusters and associations: generales
dc.subjectStars: abundanceses
dc.subjectStars: fundamental parameterses
dc.subjectStars: solar-typees
dc.titleThe Gaia -ESO Survey: A new approach to chemically characterising young open clusters: I. Stellar parameters, and iron-peak, α -, and proton-capture elementses
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcidJeffries, R. D. [0000-0001-5668-1288]-
dc.contributor.orcidMagrini, L. [0000-0003-4486-6802]-
dc.contributor.orcidMena, E. D. [0000-0003-4434-2195]-
dc.contributor.orcidSmiljanic, R. [0000-0003-0942-7855]-
dc.contributor.orcidKoposov, S. [0000-0003-2644-135X]-
dc.contributor.orcidCarraro, G. [0000-0002-0155-9434]-
dc.identifier.doi10.1051/0004-6361/201937055-
dc.identifier.e-issn1432-0746-
dc.contributor.funderEuropean Commission (EC)-
dc.contributor.funderLeverhulme Trust-
dc.contributor.funderFundacao para a Ciencia e a Tecnologia (FCT)-
dc.contributor.funderAgencia Estatal de Investigación (AEI)-
dc.description.peerreviewedPeer reviewes
dc.type.hasVersioninfo:eu-repo/semantics/publishedVersion-
dc.rights.accessRightsinfo:eu-repo/semantics/openAccess-
dc.type.coarhttp://purl.org/coar/resource_type/c_6501-
dc.relation.projectIDinfo:eu-repo/grantAgreement/EC/FP7/320360-
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