J/A+A/577/A6ivo://CDS.VizieR/J/A+A/577/A6doi:10.26093/cds/vizier.35770006CDSRauch T.Werner K.Quinet P.Kruk J.W.2017-07-11T13:08:41Z2015-04-22T08:28:19ZCDS support team

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

cds-question@unistra.fratomic-physicsFor the spectral analysis of high-resolution and high-signal-to-noise (S/N) spectra of hot stars, advanced non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These atmospheres are strongly dependent on the reliability of the atomic data that are used to calculate them. Reliable Ga IV-VI oscillator strengths are used to identify Ga lines in the spectra of the DA-type white dwarf G191-B2B and the DO-type white dwarf RE 0503-289 and to determine their photospheric Ga abundances. We newly calculated Ga IV-VI oscillator strengths to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models for analyzing of Ga lines exhibited in high-resolution and high-S/N UV observations of G191-B2B and RE 0503-289.2015A&A...577A...6Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/577/A6CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/546/A55 : Ge V and Ge VI oscillator strengths (Rauch+, 2012)J/A+A/564/A41 : Zn IV and Zn V oscillator strengths (Rauch+, 2014)J/A+A/566/A10 : Ba V, Ba VI, and Ba VII oscillator strengths (Rauch+, 2014)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/577/A6https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/577/A6http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/577/A6https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/577/A6https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/577/A6http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/577/A6GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/577/A6/GaCombined table from original tablesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonSimbad column added by the CDSphys.atmol.ionStageintnullablelambdaWavelength {lambda}0.1nmem.wldoubleE0[0/450795] Lower level, energycm**-1phys.energy;phys.atmol.levelintP0[o/e] Lower level, parityphys.atmol.parity;phys.atmol.levelcharJ0[0/6] Lower level, angular momentum quantum number Jphys.angMomentumfloatE1[224243/597358] Upper level, energycm**-1phys.energy;phys.atmol.levelintP1[o/e] Upper level, parityphys.atmol.parity;phys.atmol.levelcharJ1[0/7] Upper level, angular momentum quantum number Jphys.angMomentumfloatloggf[-4/5.5] Calculated HFR (Hartree-Fock) log(gf) value (1)phys.absorption.coefffloatgA[8e+3/3e+11] gA value (2)s**-1phys.atmol.transProbdoubleCF[-1/1] CF cancellation factor (3)phys.atmolfloat