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dc.rights.license© P. Bonifacio et al. 2020-
dc.contributor.authorBonifacio, P.-
dc.contributor.authorMolaro, P.-
dc.contributor.authorAdibekyan, V.-
dc.contributor.authorAguado, D.-
dc.contributor.authorAlibert, Y.-
dc.contributor.authorAllende Prieto, C.-
dc.contributor.authorCaffau, E.-
dc.contributor.authorCristiani, S.-
dc.contributor.authorCupani, G.-
dc.contributor.authorDi Marcoantonio, P.-
dc.contributor.authorD´Odorico, V.-
dc.contributor.authorEhrenreich, D.-
dc.contributor.authorFigueira, P.-
dc.contributor.authorGenova, R.-
dc.contributor.authorGonzález Hernández, J. I.-
dc.contributor.authorLo Curto, G.-
dc.contributor.authorLovis, C.-
dc.contributor.authorMartins, C. J. A. P.-
dc.contributor.authorMehner, A.-
dc.contributor.authorMicela, G.-
dc.contributor.authorMonaco, L.-
dc.contributor.authorNunes, N. J.-
dc.contributor.authorPepe, F. A.-
dc.contributor.authorPoretti, E.-
dc.contributor.authorRebolo, R.-
dc.contributor.authorSantos, N. C.-
dc.contributor.authorSaviane, I.-
dc.contributor.authorSousa, S.-
dc.contributor.authorSozzetti, A.-
dc.contributor.authorSuárez Mascareño, A.-
dc.contributor.authorUdry, S.-
dc.contributor.authorZapatero Osorio, M. R.-
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.accessioned2021-04-19T07:30:03Z-
dc.date.available2021-04-19T07:30:03Z-
dc.date.issued2020-01-22-
dc.identifier.citationAstronomy and Astrophysics 633: A129(2020)es
dc.identifier.issn0004-6361-
dc.identifier.otherhttps://www.aanda.org/articles/aa/full_html/2020/01/aa35833-19/aa35833-19.html-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/399-
dc.descriptionTables 1 and 2 are also available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/633/A129es
dc.description.abstractContext. The vast majority of the known stars of ultra low metallicity ([Fe/H] <  −4.5) are known to be enhanced in carbon, and belong to the “low-carbon band” (A(C) = log(C/H)+12 ≤ 7.6). It is generally, although not universally, accepted that this peculiar chemical composition reflects the chemical composition of the gas cloud out of which these stars were formed. The first ultra-metal-poor star discovered, HE 0107−5240, is also enhanced in carbon and belongs to the “low-carbon band”. It has recently been claimed to be a long-period binary, based on radial velocity measurements. It has also been claimed that this binarity may explain its peculiar composition as being due to mass transfer from a former AGB companion. Theoretically, low-mass ratios in binary systems are much more favoured amongst Pop III stars than they are amongst solar-metallicity stars. Any constraint on the mass ratio of a system of such low metallicity would shed light on the star formation mechanisms in this metallicity regime. Aims. We acquired one high precision spectrum with ESPRESSO in order to check the reality of the radial velocity variations. In addition we analysed all the spectra of this star in the ESO archive obtained with UVES to have a set of homogenously measured radial velocities. Methods. The radial velocities were measured using cross correlation against a synthetic spectrum template. Due to the weakness of metallic lines in this star, the signal comes only from the CH molecular lines of the G-band. Results. The measurement obtained in 2018 from an ESPRESSO spectrum demonstrates unambiguously that the radial velocity of HE 0107−5240 has increased from 2001 to 2018. Closer inspection of the measurements based on UVES spectra in the interval 2001–2006 show that there is a 96% probability that the radial velocity correlates with time, hence the radial velocity variations can already be suspected from the UVES spectra alone. Conclusions. We confirm the earlier claims of radial velocity variations in HE 0107−5240. The simplest explanation of such variations is that the star is indeed in a binary system with a long period. The nature of the companion is unconstrained and we consider it is equally probable that it is an unevolved companion or a white dwarf. Continued monitoring of the radial velocities of this star is strongly encouraged.es
dc.description.sponsorshipP. B. and E. C. acknowledge support from the Scientific Council of Observatoire de Paris and from the Programme National de Physique Stellaire of the Institut National des Sciences de l'Univers - CNRS. J. I. G. H. acknowledges financial support from the Spanish Ministry project MINECO AYA2017-86389-P, and also from the Spanish MINECO under the 2013 Ramon y Cajal programme MINECO RYC-2013-14875. C. J. A. P. was financed by FEDER - Fundo Europeu de Desenvolvimento Regional funds through the COMPETE 2020 - Operational Programme for Competitiveness and Internationalisation (POCI), and by Portuguese funds through FCT -Fundacao para a Ciencia e a Tecnologia in the framework of the project POCI-01-0145-FEDER-028987. N. S. was supported by FCT - Fundacao para a Ciencia e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionaliza.cao by these grants: UID/FIS/04434/2013 and POCI-01-0145-FEDER-007672; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953 and PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113. V. A. was supported by FCT through Investigador FCT contract no. IF/00650/2015/CP1273/CT0001. MRZO acknowledges financial support by the Spanish Ministry of Science, Innovation and Universities through project AYA2016-79425-C3-2-P. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project Four Aces; grant agreement No. 724427). The project has been carried out in the frame of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement; 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/AYA2017-86389-P/ES/ESPECTROSCOPIA DE ALTA RESOLUCION ORIENTADA AL ESTUDIO DE EXOTIERRAS Y LA FORMACION DE LA VIA LACTEA. EXPLOTACION CIENTIFICA DE ESPRESSO Y HORS/-
dc.relationinfo:eu-repo/grantAgreement/MINECO//RYC-2013-14875-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2016-79425-C3-2-P/ES/ENANAS MARRONES Y PLANETAS AISLADOS Y COMO COMPAÑEROS DE ESTRELLAS/-
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/4.0/-
dc.subjectBinaries: spectroscopices
dc.subjectStars: abundanceses
dc.subjectGalaxy: abundanceses
dc.subjectGalaxy: haloes
dc.titleESPRESSO highlights the binary nature of the ultra-metal-poor giant HE 0107−5240.es
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcidMolaro, P. [0000-0002-0571-4163]-
dc.contributor.orcidMonaco, L. [0000-0002-3148-9836]-
dc.contributor.orcidNunes, N. J. [0000-0002-3837-6914]-
dc.contributor.orcidSuarez Mascareño, A. [0000-0002-3814-5323]-
dc.contributor.orcidAguado, D. [0000-0001-5200-3973]-
dc.contributor.orcidGonzález Hernández, J. I. [0000-0002-0264-7356]-
dc.contributor.orcidAdibekyan, V. [0000-0002-0601-6199]-
dc.contributor.orcidZapatero Osorio, M. R. [0000-0001-5664-2852]-
dc.contributor.orcidFigueira, P. [0000-0001-8504-283X]-
dc.contributor.orcidSozzetti, A. [0000-0002-7504-365X]-
dc.contributor.orcidSantos, N. [0000-0003-4422-2919]-
dc.contributor.orcidCupani, G. [0000-0002-6830-9093]-
dc.contributor.orcidMartins, C. J. A. P. [0000-0002-4886-9261]-
dc.identifier.doi10.1051/0004-6361/201935833-
dc.identifier.e-issn1432-0746-
dc.contributor.funderAgencia Estatal de Investigación (AEI)-
dc.contributor.funderMinisterio de Economía y Competitividad (MINECO)-
dc.contributor.funderFundacao para a Ciencia e a Tecnologia (FCT)-
dc.contributor.funderEuropean Research Council (ERC)-
dc.contributor.funderEuropean Research Council (ERC)-
dc.description.peerreviewedPeer reviewes
dc.identifier.funderhttp://dx.doi.org/10.13039/501100011033-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100001871-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000781-
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/H2020/724427-
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