J/A+A/305/245ivo://CDS.VizieR/J/A+A/305/245doi:10.26093/cds/vizier.33050245CDSMagain P.Zhao G.1997-12-09T16:38:18Z1997-12-09T17:38:15ZCDS support team

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

cds-question@unistra.frchemical-abundancesline-intensitiesA detailed analysis of neutral iron lines in a sample of 13 metal-poor dwarfs and subgiants is carried out on the basis of high resolution spectra obtained with the ESO Coude Echelle Spectrometer. The deduced iron abundance is found to depend on the excitation potential of the line used, higher excitation lines generally indicating higher abundances. This could be caused by departures from the local thermodynamic equilibrium (LTE) or by temperature inhomogeneities in the stellar atmospheres. The dependency of this effect on the stellar atmospheric parameters is investigated. From the comparison of iron lines with lines of other elements, it is concluded that the low excitation Fe I lines are much more affected than the high excitation lines. The consequences of these effects for the classical abundance analyses are examined. It is found that they may explain, at least in part, some previously reported discrepancies between the results of different authors.1996A&A...305..245Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/305/245CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/305/245https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/305/245http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/305/245https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/305/245https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/305/245http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/305/245GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/305/245/table4Equivalent widths and abundancesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementElementphys.atmol.elementcharLambdaLine wavelength0.1nmem.wlfloatEW3567[]? Equivalent width for the star HD 35670.1pmspect.line.eqWidthfloatAb3567[]? Abundance for the star HD 3567 (1)phys.abundfloatEW25704[]? Equivalent width for the star HD 257040.1pmspect.line.eqWidthfloatAb25704[]? Abundance for the star HD 25704 (1)phys.abundfloatEW122196[]? Equivalent width for the star HD 1221960.1pmspect.line.eqWidthfloatAb122196[]? Abundance for the star HD 122196 (1)phys.abundfloatEW126793[]? Equivalent width for the star HD 1267930.1pmspect.line.eqWidthfloatAb126793[]? Abundance for the star HD 126793 (1)phys.abundfloatEW132475[]? Equivalent width for the star HD 1324750.1pmspect.line.eqWidthfloatAb132475[]? Abundance for the star HD 132475 (1)phys.abundfloatEW152924[]? Equivalent width for the star HD 1529240.1pmspect.line.eqWidthfloatAb152924[]? Abundance for the star HD 152924 (1)phys.abundfloatEW160617[]? Equivalent width for the star HD 1606170.1pmspect.line.eqWidthfloatAb160617[]? Abundance for the star HD 160617 (1)phys.abundfloatEW166913[]? Equivalent width for the star HD 1669130.1pmspect.line.eqWidthfloatAb166913[]? Abundance for the star HD 166913 (1)phys.abundfloatEW189558[]? Equivalent width for the star HD 1895580.1pmspect.line.eqWidthfloatAb189558[]? Abundance for the star HD 189558 (1)phys.abundfloatEW193901[]? Equivalent width for the star HD 1939010.1pmspect.line.eqWidthfloatAb193901[]? Abundance for the star HD 193901 (1)phys.abundfloatEW194598[]? Equivalent width for the star HD 1945980.1pmspect.line.eqWidthfloatAb194598[]? Abundance for the star HD 194598 (1)phys.abundfloatEW196892[]? Equivalent width for the star HD 1968920.1pmspect.line.eqWidthfloatAb196892[]? Abundance for the star HD 196892 (1)phys.abundfloatEW199289[]? Equivalent width for the star HD 1992890.1pmspect.line.eqWidthfloatAb199289[]? Abundance for the star HD 199289 (1)phys.abundfloat