J/A+A/345/430ivo://CDS.VizieR/J/A+A/345/430doi:10.26093/cds/vizier.33450430CDSHill V.1999-05-22T09:42:22Z1999-05-22T09:41:50ZCDS support team

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

cds-question@unistra.frmagellanic-cloudssupergiant-starschemical-abundancesNGC 330 is the brightest SMC young cluster and contains many bright supergiants. This cluster has aroused special interest, since the earlier abundance determinations indicated an abundance lower by a factor 5 than in the SMC field young population. In this Paper we analyse high resolution spectra of 6 cool supergiants in NGC 330, and compare in an homogeneous way, the metallicity and abundance ratios of various elements in NGC 330 and in the field of the SMC. The following Table is the Apendix to this Paper, giving the line list used in the analysis, together with the measured equivalent width and the derived abundance for each of the 6 stars.1999A&A...345..430Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/345/430CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/324/435 : Chemical composition of 6 K supergiants in the SMC (Hill 1997)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/345/430https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/345/430http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/345/430https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/345/430https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/345/430http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/345/430GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/345/430/appendixLine by line elemental abundancesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLambdaCentral wavelength of the line0.1nmem.wl.centralfloatElElementphys.atmol.elementcharDegIonDegree of Ionisationphys.atmol.ionizationintXex? Exitation potential of the lineeVphys.energy;phys.atmol.excitationfloatnullableloggf? Oscillator strength of the linephys.atmol.wOscStrengthfloatnullableEWA3? Equivalent width in Cl* NGC 330 Rob A30.1pmspect.line.eqWidthfloatnullablen_EWA3[*] Note on EWA3 (1)meta.notechar[X/H]A3? Derived abundance for Cl* NGC 330 Rob A3Sunphys.abundfloatnullableEWA6? Equivalent width in Cl* NGC 330 Rob A60.1pmspect.line.eqWidthfloatnullablen_EWA6[*] Note on EWA6 (1)meta.notechar[X/H]A6? Derived abundance for Cl* NGC 330 Rob A6Sunphys.abundfloatnullableEWA7? Equivalent width in Cl* NGC 330 Rob A70.1pmspect.line.eqWidthfloatnullablen_EWA7[*] Note on EWA7 (1)meta.notechar[X/H]A7? Derived abundance for Cl* NGC 330 Rob A7Sunphys.abundfloatnullableEWA14? Equivalent width in Cl* NGC 330 Rob A140.1pmspect.line.eqWidthfloatnullablen_EWA14[*] Note on EWA14 (1)meta.notechar[X/H]A14? Derived abundance for Cl* NGC 330 Rob A14Sunphys.abundfloatnullableEWA45? Equivalent width in Cl* NGC 330 Rob A450.1pmspect.line.eqWidthfloatnullablen_EWA45[*] Note on EWA45 (1)meta.notechar[X/H]A45? Derived abundance for Cl* NGC 330 Rob A45Sunphys.abundfloatnullableEWB40? Equivalent width in Cl* NGC 330 Rob B400.1pmspect.line.eqWidthfloatnullablen_EWB40[*] Note on EWB40 (1)meta.notechar[X/H]B40? Derived abundance for Cl* NGC 330 Rob B40Sunphys.abundfloatnullable