J/MNRAS/441/3127ivo://CDS.VizieR/J/MNRAS/441/3127doi:10.26093/cds/vizier.74413127CDSRuffoni M.P.Den Hartog E.A.Lawler J.E.Brewer N.R.Lind K.Nave G.,Pickering J.C.2024-08-09T20:15:07Z2014-10-06T14:51:27ZCDS support team

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

cds-question@unistra.fratomic-physicsspectroscopyThe Gaia-ESO Public Spectroscopic Survey (GES) is conducting a large-scale study of multi-element chemical abundances of some 100000 stars in the Milky Way with the ultimate aim of quantifying the formation history and evolution of young, mature and ancient Galactic populations. However, in preparing for the analysis of GES spectra, it has been noted that atomic oscillator strengths of important FeI lines required to correctly model stellar line intensities are missing from the atomic data base. Here, we present new experimental oscillator strengths derived from branching fractions and level lifetimes, for 142 transitions of FeI between 3526 and 10864{AA}, of which at least 38 are urgently needed by GES. We also assess the impact of these new data on solar spectral synthesis and demonstrate that for 36 lines that appear unblended in the Sun, Fe abundance measurements yield a small line-by-line scatter (0.08dex) with a mean abundance of 7.44dex in good agreement with recent publications.2014MNRAS.441.3127Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/441/3127CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/441/3127https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/441/3127http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/441/3127https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/441/3127https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/441/3127http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/441/3127GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/MNRAS/441/3127/table3Experimental branching fractions, transition probabilities, and log(gf)s for the FeI levels listed in table 2 of the paperrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintState[A-L] State (G1)phys.atmol.configurationcharLevelLower Levelphys.atmol.qnNote[*] Wavenumber from our spectra (G2)meta.notecharlam.Air[2722/13261] Transition air wavelength ({AA})0.1nmem.wl;phys.atmol.transitiondoubleprimarysigma[7539/36727] Transition wavenumber {sigma}cm**-1em.freqdoubleSSimbad column added by the CDSmeta.ref.urlcharBF[0/1]? Branching fraction (1)phys.atmol.branchingRatiofloatnullablee_BF? Precentage uncertainty in branching fraction%stat.errorfloatnullableAul? Transition probability1e-06s**-1phys.atmol.transProbfloatnullableloggf? Oscillator strength measured in this workphys.atmol.oscStrengthfloatnullablee_loggf? Uncertainty in oscillator strengthstat.error;phys.absorption.coefffloatnullableloggf0? Best previously published oscillator strengthmeta.ref;phys.atmol.oscStrength;meta.modelledfloatnullablee_loggf0? Uncertainty in loggf0 (G3)stat.errorfloatnullableq_loggf0[DE+ ] Uncertainty flag on loggf0 (G3)meta.code.qualcharr_loggf0Reference to source of loggf0 (G4)meta.ref;pos.framecharGES'Yes' if the line is a GES target (Gaia-ESO public Spectroscopic survey)meta.notecharJ/MNRAS/441/3127/table4Lines measured in previous studies, or predicted to have a BF greater than 1%, that were omitted from the BF measurements shown in table 3recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintState[A-L] State (G1)phys.atmol.configurationcharLevelLower Levelphys.atmol.qnNote[*] Wavenumber from our spectra (G2)meta.notecharlam.Air[2722/13261] Transition air wavelength ({AA})0.1nmem.wl;phys.atmol.transitiondoublesigma[7539/36727] Transition wavenumber {sigma}cm**-1em.freqdoubleloggf0Best previously published oscillator strengthmeta.ref;phys.atmol.oscStrength;meta.modelledfloate_loggf0? Uncertainty in loggf0 (G3)stat.errorfloatnullableq_loggf0[DE] Uncertainty flag on loggf0 (G3)meta.code.qualcharr_loggf0Reference to source of loggf0 (G4)meta.ref;pos.framecharl_BFp[<] Contains '<' if BFp is less than 0.001meta.code.errorcharBFp[0/1] Predicted branching fractionphys.atmol.branchingRatiofloatReasonReason for omission of the linemeta.notecharBlendList of blended lines when Reason='Blended' (1)meta.noteJ/MNRAS/441/3127/table5Lines from table 3 selected for solar analysisrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlam.Air[4423/10864] Transition air wavelength ({AA})0.1nmem.wl;phys.atmol.transitiondoublechiLower level transition energy {chi}eVphys.energy;phys.atmol.levelfloatVdWVan der Waals damping parameter (1)stat.paramdoubleloggfOscillator strength measured in this workphys.atmol.oscStrengthfloate_loggfUncertainty in oscillator strengthstat.error;phys.absorption.coefffloatloggf0Best previously published oscillator strengthmeta.ref;phys.atmol.oscStrength;meta.modelledfloate_loggf0? Uncertainty in loggf0 (G3)stat.errorfloatnullableq_loggf0[DE] Uncertainty flag on loggf0 (G3)meta.code.qualcharr_loggf0Reference to source of loggf0 (G4)meta.ref;pos.framecharepsSolar iron abundance, log{epsilon}(Fe), obtained for this line using loggfphys.abund.Fefloateps0Solar iron abundance, log{epsilon}(Fe), obtained for this line using loggf0phys.abund.Fefloat