J/A+A/567/A72ivo://CDS.VizieR/J/A+A/567/A72doi:10.26093/cds/vizier.35670072CDSGruyters P.Nordlander T.Korn A.J.2015-01-11T15:44:48Z2014-07-15T07:13:13ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frchemical-abundancesglobular-star-clustersastronomical-modelsstellar-atmospheresvisible-astronomymedium-band-photometryspectroscopyAbundance trends in heavier elements with evolutionary phase have been shown to exist in the globular cluster NGC 6752. These trends are a result of atomic diffusion and additional (non-convective) mixing. Studying such trends can provide us with important constraints on the extent to which diffusion modifies the internal structure and surface abundances of solar-type, metal-poor stars. Taking advantage of a larger data sample, we investigate the reality and the size of these abundance trends and address questions and potential biases associated with the various stellar populations that make up NGC 6752. We perform an abundance analysis by combining photometric and spectroscopic data of 194 stars located between the turnoff point and the base of the red giant branch. Stellar parameters are derived from uvby Stromgren photometry. Using the quantitative-spectroscopy package SME, stellar surface abundances for light elements such as Li, Na, Mg, Al, and Si as well as heavier elements such as Ca, Ti, and Fe are derived in an automated way by fitting synthetic spectra to individual lines in the stellar spectra, obtained with the VLT/FLAMES-GIRAFFE spectrograph. Based on uvby Stromgren photometry, we are able to separate three stellar populations in NGC 6752 along the evolutionary sequence from the base of the red giant branch down to the turnoff point. We find weak systematic abundance trends with evolutionary phase for Ca, Ti, and Fe which are best explained by stellar-structure models including atomic diffusion with efficient additional mixing. We derive a new value for the initial lithium abundance of NGC 6752 after correcting for the effect of atomic diffusion and additional mixing which falls slightly below the predicted standard BBN value. We find three stellar populations by combining photometric and spectroscopic data of 194 stars in the globular cluster NGC 6752. Abundance trends for groups of elements, differently affected by atomic diffusion and additional mixing, are identified. Although the statistical significance of the individual trends is weak, they all support the notion that atomic diffusion is operational along the evolutionary sequence of NGC 6752.2014A&A...567A..72Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/567/A72CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/490/777 : Abundances of Population II stars in NGC 6397 (Lind+, 2008)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/567/A72https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/567/A72http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/567/A72https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/567/A72https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/567/A72http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/567/A72GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/567/A72/stars (Stars observed: Coordinates, photometry, spectrum S/N, stellar parameters, abundances of anticorrelated elements, and photometric assignments of chemical populations)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/567/A72/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/567/A72/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/567/A72/stars?GETtext/xml+votable180.050000true287.75077083-60.02249750.0055555555555555566/47125 47168https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/567/A72?format=asciiOpticaldefaultJ/A+A/567/A72/starsStars observed: Coordinates, photometry, spectrum S/N, stellar parameters, abundances of anticorrelated elements, and photometric assignments of chemical populationsymagStromgren y magnitudemagphot.mag;em.opt.VfloatNameStar number (C6752-NNNN)meta.id;meta.mainintprimaryRAJ2000Right ascension (J2000.0)pos.eq.ra;meta.mainDEJ2000Declination (J2000.0)pos.eq.dec;meta.mainumagStromgren u magnitudemagphot.mag;em.opt.UfloatvmagStromgren v magnitudemagphot.mag;em.opt.BfloatbmagStromgren b magnitudemagphot.mag;em.opt.BfloatSNR9S/N of HR9 (5143-5356{AA})stat.snrintSNR10S/N in HR10 (5339-5619{AA})stat.snrintSNR11S/N in HR11 (5597-5840{AA})stat.snrintSNR15S/N in HR15 (6607-6965{AA})stat.snrintTeffEffective temperatureKphys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloatxiMicroturbulence parameter {xi}km/sstat.paramfloatl_A(Li)? Limit flag on A(Li)meta.code.errorcharA(Li)[0.4/2.5]? Lithium abundance (1)phys.abundfloatnullablee_A(Li)? Uncertainty in A(Li) (2)stat.errorfloatnullablel_[Na/Fe]Limit flag on [Na/Fe]meta.code.error;phys.abundchar[Na/Fe][-0.7/0.7]? Abundance ratio Na over Fe (1)log(Sun)phys.abund.Fefloatnullablee_[Na/Fe]? Uncertainty in [Na/Fe] (2)log(Sun)stat.error;phys.abundfloatnullablel_[Mg/Fe]Limit flag on [Mg/Fe]meta.code.error;phys.abundchar[Mg/Fe][0/0.5]? Abundance ratio Mg over Fe (1)log(Sun)phys.abund.Fefloatnullablee_[Mg/Fe]? Uncertainty in [Mg/Fe] (2)log(Sun)stat.error;phys.abundfloatnullablel_[Al/Fe]Limit flag on [Al/Fe]meta.code.error;phys.abundchar[Al/Fe][-1.5/0.9]? Abundance ratio Al over Fe (1)log(Sun)phys.abund.Fefloatnullablee_[Al/Fe]? Uncertainty in [Al/Fe] (2)log(Sun)stat.error;phys.abundfloatnullablel_[Si/Fe]Limit flag on [Si/Fe]meta.code.error;phys.abundchar[Si/Fe][-1.0/0.8]? Abundance ratio Si over Fe (1)log(Sun)phys.abund.Fefloatnullablee_[Si/Fe]? Uncertainty in [Si/Fe] (2)log(Sun)stat.error;phys.abundfloatnullablel_A(Fe)Limit flag on A(Fe)meta.code.errorcharA(Fe)[5.3/6.0] Iron abundance (1)phys.abund.Fefloate_A(Fe)Uncertainty in A(Fe) (2)stat.errorfloatPop[PIE] Chemical population flag: P=primordial, I=intermediaten E=extrememeta.code.memberchar