J/A+A/360/499ivo://CDS.VizieR/J/A+A/360/499doi:10.26093/cds/vizier.33600499CDSTautvaisiene G.Edvardsson B.Tuominen I.Ilyin I.2000-10-11T11:54:08Z2000-10-11T11:54:00ZCDS support team

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

cds-question@unistra.fropen-star-clustersline-intensitiesHigh-resolution spectra of six core helium-burning `clump' stars and three giants in the open cluster M 67 have been obtained with the SOFIN spectrograph on the Nordic Optical Telescope to investigate abundances of up to 25 chemical elements. Abundances of carbon were studied using the C_2_ Swan (0,1) band head at 5635.5{AA}. The wavelength interval 7980-8130{AA} with strong CN features was analysed in order to determine nitrogen abundances and ^12^C/^13^C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300{AA}. The overall metallicity of the cluster stars was found to be close to solar ([Fe/H]=-0.03+/-0.03). Compared with the Sun and other dwarf stars of the Galactic disk, as well as with dwarf stars of M 67 itself, abundances in the investigated stars suggest that carbon is depleted by about 0.2dex, nitrogen is enhanced by about 0.2dex and oxygen is unaltered. Among other mixing-sensitive chemical elements an overabundance of sodium may be suspected. The mean C/N and ^12^C/^13^C ratios are lowered to the values of 1.7+/-0.2 and 24+/-4 in the giants and to the values of 1.4+/-0.2 and 16+/-4 in the clump stars. These results suggest that extra mixing of CN-cycled material to the stellar surface takes place after the He-core flash. Abundances of heavy chemical elements in all nine stars were found to be almost identical and close to solar.2000A&A...360..499Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/360/499CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/AJ/112/628 : Deep Wide-Field Spectrophotometry of M67 (Fan+ 1996)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/360/499https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/360/499http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/360/499https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/360/499https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/360/499http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/360/499GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/360/499/table2Equivalent widths of lines measured from spectra of resolving power 60000recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementLine identification: chemical element and ionisation stage (e.g. 23.01 means singly ionised vanadium, i.e. V II)meta.idfloatLambdaWavelength (Angstroms)0.1nmem.wlfloatEWF84? Equivalent width for the clump star F84pmspect.line.eqWidthfloatnullableEWF141Equivalent width for the clump star F141pmspect.line.eqWidthfloatEWF151Equivalent width for the clump star F151pmspect.line.eqWidthfloatJ/A+A/360/499/table3Equivalent widths of lines measured from spectra of resolving power 30000recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementLine identification: chemical element and ionisation stage (e.g. 23.01 means singly ionised vanadium, i.e. V II)meta.idfloatLambdaWavelength (Angstroms)0.1nmem.wlfloatEWF84? Equivalent width for the clump star F84pmspect.line.eqWidthfloatnullableEWF105Equivalent width for the giant star F105pmspect.line.eqWidthfloatEWF108Equivalent width for the giant star F108pmspect.line.eqWidthfloatEWF141Equivalent width for the clump star F141pmspect.line.eqWidthfloatEWF151Equivalent width for the clump star F151pmspect.line.eqWidthfloatEWF164Equivalent width for the clump star F164pmspect.line.eqWidthfloatEWF170Equivalent width for the giant star F170pmspect.line.eqWidthfloatEWF224Equivalent width for the clump star F224pmspect.line.eqWidthfloatEWF266Equivalent width for the clump star F266pmspect.line.eqWidthfloat