J/MNRAS/376/361ivo://CDS.VizieR/J/MNRAS/376/361doi:10.26093/cds/vizier.73760361CDSFolsom C.P.Wade G.A.Bagnulo S.Landstreet J.D.2024-07-04T20:18:07Z2007-12-28T22:23:59ZCDS support team

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

cds-question@unistra.fropen-star-clusterspeculiar-variable-starschemical-abundancesThe connection between age, rotation and chemical abundance of magnetic Ap stars is poorly understood. Using open clusters, we are able to study samples of stars that are both coeval and co-environmental. By determining rotation and chemical abundance for Ap star members of clusters with various ages, the variations of these properties as a function of age and environment can be derived. All four probable Ap star members of the open cluster NGC 6475, as well as one normal late B star, were studied using detailed spectrum synthesis of high-resolution UVES-POP spectra. Probable cluster membership was confirmed for all five stars; however, chemical abundance anomalies only appear to be present in spectra of three. Projected rotational velocity and chemical abundances for 21 elements ranging from C to Eu are presented for the five stars. In the three peculiar stars, we find overabundances of Si, Cr, Mn, Fe and rare earths, such as Nd, characteristic of Ap stars. The set of chemically peculiar stars show fairly homogeneous abundance tables, however, notable differences exist for a few elements. There also exist appreciable differences in the vsini and main-sequence evolutionary stage of the chemically peculiar stars. This may hint at the underlying processes giving rise to the observed abundance anomalies. With this first detailed study of chemical abundances of a complete sample of magnetic Ap/Bp stars in an open cluster, we have initiated an exploration of the environmental and evolutionary influence on chemical peculiarity.2007MNRAS.376..361Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/376/361CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/376/361https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/376/361http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/376/361https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/376/361https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/376/361http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/376/361GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/MNRAS/376/361/linesAtomic line data used for the studied starsElElementphys.atmol.elementcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTSimbad column added by the CDSmeta.id;meta.datasetcharStateIonization State (1=neutral)physintlambdaWavelength0.1nmem.wldoublelog(gf)Oscillator Strengthphys.atmol.oscStrengthfloatElowLower Level EnergyeVphys.energy;phys.atmol.levelfloat