J/MNRAS/537/3054ivo://CDS.VizieR/J/MNRAS/537/3054doi:10.26093/cds/vizier.75373054CDSCay M.T.Cay I.H.Civelekler B.2025-03-07T20:14:50Z2025-02-19T09:01:31ZCDS support team

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

cds-question@unistra.fram-starschemically-peculiar-starsline-intensitiesUnderstanding the evolution of metallic-line (Am) stars requires well determined atmospheric parameters and abundance patterns of the selected candidates. In this study, we presented a detailed abundance analysis of 15 Vul (HD 189849), identified as a marginal star, using a combination of equivalent width and spectrum synthesis techniques, under the LTE assumption. We compared our findings to previous analyses of the star, providing critique on both their results and our own. Our results suggest that although 15 Vul exhibits some underabundances of calcium and scandium, which are typically associated with stars, it might be more accurately identified as a normal A star in terms of its abundance pattern of all other elements and microturbulence velocity. The stars position on the HR diagram, along with our findings, may indicate that it is potentially a classical star that has evolved into the subgiant phase as a quasi-normal star. This may be the first identification of an evolved star.2025MNRAS.537.3054Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/537/3054CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/537/3054https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/537/3054http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/537/3054https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/537/3054https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/537/3054http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/537/3054GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/MNRAS/537/3054/table1The lines and the related data used in the analysis with individual abundance resultsr_HFSReferences to HFS data (1)meta.bibcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelenght of the line (in Angstroem)0.1nmem.wldoubleLEPLow Excitation PotentialeVphys.atmol.excitationfloatloggfLogarithm of weighted oscillator strengthphys.atmol.oscStrengthfloatEW? Equivalent width (in miliAngstroem)0.1pmspect.line.eqWidthfloatnullable[Nel/H]Abundance relative to Sun. [Nel/H]=log(Nel/H)_star_-log(Nel/H)_sun_phys.abundfloatr_loggfReferences to loggf data (1)meta.bibcharIonSymbol of the ionphys.atmol.ionStagecharMethodMethod of analysis (Equivalent Width or Spectrum Synthesis)meta.notechar