J/A+A/572/A108ivo://CDS.VizieR/J/A+A/572/A108doi:10.26093/cds/vizier.35720108CDSThygesen A. O.Sbordone L.Andrievsky S.Korotin S.Yong D.Zaggia S.,Ludwig H.-G.Collet R.Asplund M.Ventura P.D'Antona F.Melendez J.,D'Ercole A.2015-05-02T10:36:31Z2014-12-04T09:17:04ZCDS support team

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

cds-question@unistra.frmilky-way-galaxyglobular-star-clusterschemical-abundancesgiant-starsradial-velocityThe study of chemical abundance patterns in globular clusters is of key importance to constrain the different candidates for intra-cluster pollution of light elements. We aim at deriving accurate abundances for a large range of elements in the globular cluster 47 Tucanae (NGC 104) to add new constraints to the pollution scenarios for this particular cluster, expanding the range of previously derived element abundances. Using tailored 1D LTE atmospheric models together with a combination of equivalent width measurements, LTE, and NLTE synthesis we derive stellar parameters and element abundances from high-resolution, high signal-to-noise spectra of 13 red giant stars near the tip of the RGB. We derive abundances of a total 27 elements (O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr, Mo, Ru, Ba, La, Ce, Pr, Nd, Eu, Dy). Departures from LTE were taken into account for Na, Al and Ba. We find a mean [Fe/H]=-0.78+/-0.07 and [alpha/Fe]=0.34+/-0.03 in good agreement with previous studies. The remaining elements show good agreement with the literature, but the inclusion of NLTE for Al has a significant impact on the behaviour of this key element. We confirm the presence of an Na-O anti-correlation in 47 Tucanae found by several other works. Our NLTE analysis of Al shifts the [Al/Fe] to lower values, indicating that this may be overestimated in earlier works. No evidence for an intrinsic variation is found in any of the remaining elements.2014A&A...572A.108Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/572/A108CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/435/657 : Equivalent widths of 5 giants in 47 Tuc (Alves-Brito+, 2005)J/A+A/550/A34 : Abundances of red giants in M4 and 47 Tuc (Carretta+, 2013)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/572/A108https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/572/A108http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/572/A108https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/572/A108https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/572/A108http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/572/A108GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/572/A108/stars (Properties of the observed targets (table1), fundamental stellar parameters (table 8), and abundances (table9))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/572/A108/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/572/A108/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/572/A108/stars?GETtext/xml+votable180.050000true6.0187917-71.95309440.0055555555555555566/33321 33323https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/572/A108?format=asciiOpticaldefaultJ/A+A/572/A108/starsProperties of the observed targets (table1), fundamental stellar parameters (table 8), and abundances (table9)IDID numbermeta.id;meta.mainintNFeINumber of lines usedmeta.numberintNNaNumber of lines usedmeta.numberintNSiNumber of lines usedmeta.numberintNEuIINumber of lines usedmeta.numberintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintn_ID[*] * indicates polluted targetmeta.notecharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainVmagV magnitude (1)magphot.mag;em.opt.VfloatBmagB magnitude (1)magphot.mag;em.opt.BfloatImagI magnitude (1)magphot.mag;em.opt.IfloatUmagU magnitude (1)magphot.mag;em.opt.UfloatRV[-29/-9] Radial velocitykm/sphys.veloc;pos.heliocentricfloate_RV[0.1/0.4] rms uncertainty of RVkm/sstat.errorfloatTeffEffective temperatureKphys.temperature.effectiveintlogg[0.3/1.45] Surface gravitylog(cm.s**-2)phys.gravityfloatVt[1.1/1.9] Microturbulent velocity {xi}_t_km/sphys.velocfloat[Fe/H][-0.86/-0.66] Metallicity [Fe/H]log(Sun)phys.abund.ZfloatVmac[5/7] Macroturbulent velocitykm/sphys.velocfloat[FeI/H]Abundance (26.0)log(Sun)phys.abundfloate_[FeI/H]Uncertainty on measurementlog(Sun)stat.error;phys.abundfloat[FeII/H]Abundance (26.1)log(Sun)phys.abundfloate_[FeII/H]Uncertainty on measurementlog(Sun)stat.error;phys.abundfloatNFeIINumber of lines usedmeta.numberint[O/Fe]? Abundance ratio (8.)log(Sun)phys.abundfloatnullablee_[O/Fe]? Uncertainty on measurementlog(Sun)phys.abundfloatnullableNONumber of lines usedmeta.numberint[Na/Fe]Abundance ratio (11.)log(Sun)phys.abundfloate_[Na/Fe]Uncertainty on measurementlog(Sun)phys.abundfloat[Mg/Fe]Abundance ratio (12.)log(Sun)phys.abundfloate_[Mg/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNMgNumber of lines usedmeta.numberint[Al/Fe]Abundance ratio (13.)log(Sun)phys.abundfloate_[Al/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNAlNumber of lines usedmeta.numberint[Si/Fe]Abundance ratio (14.)log(Sun)phys.abundfloate_[Si/Fe]Uncertainty on measurementlog(Sun)phys.abundfloat[Ca/Fe]Abundance ratio (20.)log(Sun)phys.abundfloate_[Ca/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNCaNumber of lines usedmeta.numberint[ScI/Fe]Abundance ratio (21.0)log(Sun)phys.abundfloate_[ScI/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNScINumber of lines usedmeta.numberint[ScII/Fe]Abundance ratio (21.1)log(Sun)phys.abundfloate_[ScII/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNScIINumber of lines usedmeta.numberint[TiI/Fe]Abundance ratio (22.0)log(Sun)phys.abundfloate_[TiI/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNTiINumber of lines usedmeta.numberint[TiII/Fe]Abundance ratio (22.1)log(Sun)phys.abundfloate_[TiII/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNTiIINumber of lines usedmeta.numberint[V/Fe]Abundance ratio (23.)log(Sun)phys.abundfloate_[V/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNVNumber of lines usedmeta.numberint[Cr/Fe]Abundance ratio (24.)log(Sun)phys.abundfloate_[Cr/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNCrNumber of lines usedmeta.numberint[Mn/Fe]Abundance ratio (25.)log(Sun)phys.abundfloate_[Mn/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNMnNumber of lines usedmeta.numberint[Co/Fe]Abundance ratio (27.)log(Sun)phys.abundfloate_[Co/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNCoNumber of lines usedmeta.numberint[Ni/Fe]Abundance ratio (28.)log(Sun)phys.abundfloate_[Ni/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNNiNumber of lines usedmeta.numberint[Cu/Fe]Abundance ratio (29.)log(Sun)phys.abundfloate_[Cu/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNCuNumber of lines usedmeta.numberint[Zn/Fe]Abundance ratio (30.)log(Sun)phys.abundfloate_[Zn/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNZnNumber of lines usedmeta.numberint[YII/Fe]Abundance ratio (39.2)log(Sun)phys.abundfloate_[YII/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNYIINumber of lines usedmeta.numberint[Zr/Fe]Abundance ratio (40.)log(Sun)phys.abundfloate_[Zr/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNZrNumber of lines usedmeta.numberint[Mo/Fe]Abundance ratio (42.)log(Sun)phys.abundfloate_[Mo/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNMoNumber of lines usedmeta.numberint[Ru/Fe]Abundance ratio (44.)log(Sun)phys.abundfloate_[Ru/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNRuNumber of lines usedmeta.numberint[BaII/Fe]Abundance ratio (56.1)log(Sun)phys.abundfloate_[BaII/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNBaIINumber of lines usedmeta.numberint[LaII/Fe]Abundance ratio (57.1)log(Sun)phys.abundfloate_[LaII/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNLaIINumber of lines usedmeta.numberint[CeII/Fe]? Abundance ratio (58.1)log(Sun)phys.abundfloatnullablee_[CeII/Fe]? Uncertainty on measurementlog(Sun)phys.abundfloatnullableNCeIINumber of lines usedmeta.numberint[PrII/Fe]Abundance ratio (59.1)log(Sun)phys.abundfloate_[PrII/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNPrIINumber of lines usedmeta.numberint[NdII/Fe]Abundance ratio (60.1)log(Sun)phys.abundfloate_[NdII/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNNdIINumber of lines usedmeta.numberint[EuII/Fe]Abundance ratio (63.1)log(Sun)phys.abundfloate_[EuII/Fe]Uncertainty on measurementlog(Sun)phys.abundfloat[DyII/Fe]Abundance ratio (66.1)log(Sun)phys.abundfloate_[DyII/Fe]Uncertainty on measurementlog(Sun)phys.abundfloatNDyIINumber of lines usedmeta.numberintJ/A+A/572/A108/table2Non-HFS lines used for abundance analysisrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[4800/6800] Wavelength {lambda} (in Angstrom)0.1nmem.wldoubleIonElement ID. XX.0 neutral, XX.1 ionized speciesphys.atmol.ionStagefloatloggfOscillator strengthphys.atmol.oscStrengthfloatElowLower excitation potentialeVphys.atmol.excitation;stat.minfloatJ/A+A/572/A108/table5Hyperfine structure (HFS) linelist, split into components (except Ba)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[4800/6800] Wavelength {lambda} (in Angstrom)0.1nmem.wldoubleIonElement ID. XX.0 neutral, XX.1 ionized speciesphys.atmol.ionStagefloatloggfOscillator strengthphys.atmol.oscStrengthfloatElowLower excitation potentialeVphys.atmol.excitation;stat.minfloat