J/A+A/668/A49ivo://CDS.VizieR/J/A+A/668/A49doi:10.26093/cds/vizier.36680049CDSFranciosini E.Randich S.de Laverny P.Biazzo K.Feuillet D.K.,Frasca A.Lind K.Prisinzano L.Tautvaisiene G.Lanzafame A.C.,Smiljanic R.Gonneau A.Magrini L.Pancino E.Guiglion G.Sacco G.G.,Sanna N.Gilmore G.Bonifacio P.Jeffries R.D.Micela M.Prusti T.,Alfaro E.J.Bensby T.Bragaglia A.Francois P.Korn A.J.Van Eck S.,Bayo A.Bergemann M.Carraro G.Heiter U.Hourihane A.Jofre P.,Lewis J.Martayan C.Monaco L.Morbidelli L.Worley C.C.Zaggia S.2024-11-06T20:01:48Z2022-12-01T08:31:27ZCDS support team

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

cds-question@unistra.frlate-type-starschemical-abundancesspectroscopyThe Gaia-ESO Survey (GES) is a large public spectroscopic survey that was carried out using the multi-object FLAMES spectrograph at the VLT. The survey provides accurate radial velocities, stellar parameters and elemental abundances for ~115000 stars in all Milky Way components. In this paper we describe the method adopted in the final data release to derive lithium equivalent widths (EWs) and abundances. Lithium EWs were measured using two different approaches for FGK and M-type stars, to account for the intrinsic differences in the spectra. For FGK stars we fitted the lithium line using Gaussian components, while direct integration over a predefined interval was adopted for M-type stars. Care was taken to ensure continuity between the two regimes. Abundances were derived using a new set of homogeneous curves of growth that were derived specifically for GES, and were measured on a synthetic spectral grid consistently with the way the EWs were measured. The derived abundances were validated by comparison with those measured by other analysis groups using different methods. Lithium EWs were measured for ~40000 stars, and abundances could be derived for ~38000 of them. The vast majority of the measures (80%) have been obtained for stars in open cluster fields. The remaining objects are stars in globular clusters, or field stars in the Milky way disc, bulge and halo. The GES dataset of homogeneous lithium abundances described here will be valuable for our understanding of several processes, from stellar evolution and internal mixing in stars at different evolutionary stages to Galactic evolution.2022A&A...668A..49Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/668/A49CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/668/A49https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/668/A49http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/668/A49https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/668/A49https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/668/A49http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/668/A49GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/668/A49/tablea1Lithium curves of growth for FGK starsTeff[4000/8000] Effective temperatureKphys.temperature.effectivefloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogg[0.5/5.0] Surface gravitylog(cm.s**-2)phys.gravityfloat[Fe/H][-2.5/0.5] Metallicityphys.abund.ZfloatA(Li)[-1.0/4.0] Lithium abundancephys.abundfloatEW(Li)Lithium equivalent width (mAngstroem)0.1pmspect.line.eqWidthfloatJ/A+A/668/A49/tablea2Blend corrections for FGK starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeff[4000/8000] Effective temperatureKphys.temperature.effectivefloatlogg[0.5/5.0] Surface gravitylog(cm.s**-2)phys.gravityfloat[Fe/H][-2.5/0.5] Metallicityphys.abund.ZfloatEW(Fe)Equivalent width of Fe blend (mAngstroem)0.1pmspect.line.eqWidthfloatJ/A+A/668/A49/tablea3Lithium curves of growth for M-type starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeff[3000/4500] Effective temperatureKphys.temperature.effectivefloatlogg[0.5/5.0] Surface gravitylog(cm.s**-2)phys.gravityfloat[Fe/H][-1.5/0.5] Metallicityphys.abund.ZfloatvsiniProjected rotational velocitykm/sphys.veloc.rotatfloatA(Li)[-1.0/4.0] Lithium abundancephys.abundfloatpEWLithium pesudo-equivalent width (mAngstroem)0.1pmspect.line.widthfloat