J/A+A/671/A124ivo://CDS.VizieR/J/A+A/671/A124doi:10.26093/cds/vizier.36710124CDSMucciarelli A.Minelli A.Bellazzini M.Lardo C.Romano D.Origlia L.,Ferraro F.R.2024-08-05T20:00:59Z2023-03-15T08:47:00ZCDS support team

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

cds-question@unistra.frmagellanic-cloudsgiant-starschemical-abundancesspectroscopyvisible-astronomyWe present the chemical composition of 206 red giant branch stars members of the Small Magellanic Cloud (SMC) using optical, high-resolution spectra collected with the multi-object spectrograph FLAMES-GIRAFFE at the ESO Very Large Telescope. This sample includes stars in three fields located in different positions within the parent galaxy. We analysed the main groups of elements, namely light- (Na), {alpha}- (O, Mg, Si, Ca, Ti), iron-peak (Sc, V, Fe, Ni, Cu) and s-process elements (Zr, Ba, La). The metallicity distribution of the sample displays a main peak around [Fe/H]~-1 --- and a weak metal-poor tail. However, the three fields display [Fe/H] distributions different with each other, in particular a difference of 0.2 --- is found between the mean metallicities of the two most internal fields. The fraction of metal-poor stars increases significantly (from ~1 to ~20%) from the innermost fields to the most external one, likely reflecting an age gradient in the SMC. Also, we found a hint of possible chemically/kinematic distinct substructures. The SMC stars have abundance ratios clearly distinct with respect to the Milky Way stars, in particular for the elements produced by massive stars (like Na, {alpha} and most iron-peak elements) that have abundance ratios systematically lower than those measured in our Galaxy. This points out that the massive stars contributed less to the chemical enrichment of the SMC with respect to the Milky Way, according to the low star formation rate expected for this galaxy. Finally, we identified small systematic differences in the abundances of some elements (Na, Ti, V and Zr) in the two innermost fields, suggesting that the chemical enrichment history in the SMC has been not uniform.2023A&A...671A.124Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/671/A124CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/671/A124https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/671/A124http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/671/A124https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/671/A124https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/671/A124http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/671/A124GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/671/A124/table2 (Main information of the observed targets)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/671/A124/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/671/A124/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/671/A124/table2?GETtext/xml+votable180.050000true6.6427941-71.52930470.0055555555555555566/33287 33293 33304 33306 33323 33326https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/671/A124?format=asciiOpticaldefaultJ/A+A/671/A124/table2Main information of the observed targetsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar name (FLD-NNN_NNNNNN)meta.id;meta.maincharGaiaEDR3Gaia EDR3 identification numbermeta.idRA_ICRSRight ascension (ICRS) at Ep=2016.0degpos.eq.ra;meta.mainDE_ICRSDeclination (ICRS) at Ep=2016.0degpos.eq.dec;meta.mainRVHeliocentric radial velocitykm/sspect.dopplerVeloc;pos.heliocentricfloate_RVUncertainty on radial velocitykm/sstat.errorfloatSimbadSimbad column added by the CDSmeta.ref.urlcharTeffEffective temperatureKphys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloatvtMicroturbulent velocitykm/sphys.velocfloat[Fe/H]Abundance relative to the Sun for FeIphys.abundfloate_[Fe/H]Uncertainty on the abundance for FeIstat.error;phys.abund.FefloatJ/A+A/671/A124/table3Main information of the used atomic linesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelength10nmem.wldoubleElChemical elementphys.atmol.elementcharIonIonization stagephys.atmol.ionStagecharloggflog of oscillator strengthphys.atmol.oscStrengthfloatchiExcitation potentialeVphys.atmol.excitationfloatr_loggfReference of the loggf (1)meta.ref;pos.framecharJ/A+A/671/A124/table5Chemical abundances of the observed targetse_[Ni/Fe]? Uncertainty on the abundance for NiIstat.error;phys.abundfloatnullable[Cu/Fe]? Abundance relative to the Sun for CuIphys.abundfloatnullablee_[Cu/Fe]? Uncertainty on the abundance for CuIstat.error;phys.abundfloatnullablel_[Cu/Fe][0/1] Upper limit for CuI (1)meta.code.error;phys.abundchar[Zr/Fe]? Abundance relative to the Sun for ZrIphys.abundfloatnullablee_[Zr/Fe]? Uncertainty on the abundance for ZrIstat.error;phys.abundfloatnullablel_[Zr/Fe][0/1] Upper limit for ZrI (1)meta.code.error;phys.abundchar[Ba/Fe]? Abundance relative to the Sun for BaIIphys.abundfloatnullablee_[Ba/Fe]? Uncertainty on the abundance for BaIIstat.error;phys.abundfloatnullable[La/Fe]? Abundance relative to the Sun for LaIIphys.abundfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar name (FLD-NNN_NNNNNN)meta.id;meta.mainchar[Fe/H]Abundance relative to the Sun for FeIphys.abundfloat[O/Fe]? Abundance relative to the Sun for OIphys.abundfloatnullablee_[O/Fe]? Uncertainty on the abundance for OIstat.error;phys.abundfloatnullablel_[O/Fe][0/1] Upper limit for OI (1)meta.code.error;phys.abundchar[Na/Fe]? Abundance relative to the Sun for NaIphys.abundfloatnullablee_[Na/Fe]? Uncertainty on the abundance for NaIstat.error;phys.abundfloatnullablel_[Na/Fe][0/1] Upper limit for NaI (1)meta.code.error;phys.abundchar[Mg/Fe]? Abundance relative to the Sun for MgIphys.abundfloatnullablee_[Mg/Fe]? Uncertainty on the abundance for MgIstat.error;phys.abundfloatnullable[Si/Fe]? Abundance relative to the Sun for SiIphys.abundfloatnullablee_[Si/Fe]? Uncertainty on the abundance for SiIstat.error;phys.abundfloatnullablel_[Si/Fe][0/1] Upper limit for SiI (1)meta.code.error;phys.abundchar[Ca/Fe]? Abundance relative to the Sun for CaIphys.abundfloatnullablee_[Ca/Fe]? Uncertainty on the abundance for CaIstat.error;phys.abundfloatnullable[Sc/Fe]? Abundance relative to the Sun for ScIIphys.abundfloatnullablee_[Sc/Fe]? Uncertainty on the abundance for ScIIstat.error;phys.abundfloatnullable[Ti/Fe]? Abundance relative to the Sun for TiIphys.abundfloatnullablee_[Ti/Fe]? Uncertainty on the abundance for TiIstat.error;phys.abundfloatnullable[V/Fe]? Abundance relative to the Sun for VIphys.abundfloatnullablee_[V/Fe]? Uncertainty on the abundance for VIstat.error;phys.abundfloatnullable[Ni/Fe]? Abundance relative to the Sun for NiIphys.abundfloatnullablee_[La/Fe]? Uncertainty on the abundance for LaIIstat.error;phys.abundfloatnullablel_[La/Fe][0/1] Upper limit for LaII (1)meta.code.error;phys.abundchar