J/A+A/546/A55ivo://CDS.VizieR/J/A+A/546/A55doi:10.26093/cds/vizier.35460055CDSRauch T.Werner K.Biemont E.Quinet P.Kruk J.W.2017-06-27T06:38:44Z2012-10-04T09:13:32ZCDS support team

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

cds-question@unistra.fratomic-physicsState-of-the-art spectral analysis of hot stars by means of non-LTE model-atmosphere techniques has arrived at a high level of sophistication. The analysis of high-resolution and high-S/N spectra, however, is strongly restricted by the lack of reliable atomic data for highly ionized species from intermediate-mass metals to trans-iron elements. Especially data for the latter has only been sparsely calculated. Many of their lines are identified in spectra of extremely hot, hydrogen-deficient post-AGB stars. A reliable determination of their abundances establishes crucial constraints for AGB nucleosynthesis simulations and, thus, for stellar evolutionary theory. In a previous analysis of the UV spectrum of RE 0503-289, spectral lines of highly ionized Ga, Ge, As, Se, Kr, Mo, Sn, Te, I, and Xe were identified. Individual abundance determinations are hampered by the lack of reliable oscillator strengths. Most of these identified lines stem from Ge V. In addition, we identified Ge VI lines for the first time. We calculated Ge V and Ge VI oscillator strengths in order to reproduce the observed spectrum.2012A&A...546A..55Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/546/A55CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/546/A55https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/546/A55http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/546/A55https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/546/A55https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/546/A55http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/546/A55GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/546/A55/table2Data for GeVgAgA value (2)s**-1stat.valuedoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelength0.1nmem.wldoubleE0Lower level energycm**-1phys.energy;phys.atmol.levelintP0[e/o] lower level parity (even or odd)phys.atmol.paritycharJ0[0/6] Lower level angular momentum quantum numberphys.atmol.qnfloatE1Upper level energycm**-1phys.energy;phys.atmol.levelintP1[e/o] Upper level parity (even or odd)phys.atmol.paritycharJ1[0/6] Upper level angular momentum quantum numberphys.atmol.qnfloatloggfCalculated HFR log gf value (1)phys.absorption.coeff;meta.modelledfloatCFCF cancellation factor as defined by Cowan (1981, The theory of atomic structure and spectra, Los Alamos Series in Basic and Applied Sciences, Berkeley: University of California Press)phys.atmolfloatJ/A+A/546/A55/table4Data for GeVIrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelength0.1nmem.wldoubleE0Lower level energycm**-1phys.energy;phys.atmol.levelintP0[e/o] lower level parity (even or odd)phys.atmol.paritycharJ0[0/6] Lower level angular momentum quantum numberphys.atmol.qnfloatE1Upper level energycm**-1phys.energy;phys.atmol.levelintP1[e/o] Upper level parity (even or odd)phys.atmol.paritycharJ1[0/6] Upper level angular momentum quantum numberphys.atmol.qnfloatloggfCalculated HFR log gf value (1)phys.absorption.coeff;meta.modelledfloatgAgA value (2)s**-1stat.valuedoubleCFCF cancellation factor as defined by Cowan (1981, The theory of atomic structure and spectra, Los Alamos Series in Basic and Applied Sciences, Berkeley: University of California Press)phys.atmolfloat