J/other/PARep/2.ivo://CDS.VizieR/J/other/PARep/2.65CDSSahin T.Guney F.Senturk S.A.Cinar N.Marismak M.2025-09-18T09:06:52Z2025-09-18T09:46:38ZCDS support team

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

cds-question@unistra.frthe-suneffective-temperatureg-starschemical-abundancesspectroscopyvisible-astronomyThis study introduces a line list for the abundance analysis of F-and G-type stars across the 4,080-9,675{AA} wavelength range. A systematic search employing lower excitation potentials, accurate log gf values, and an updated multiplet table led to the identification of 592 lines across 33 species (25 elements), including C, O, Mg (ionized), Al, P, S, Cu, Zr (neutral), and La. To determine the uncertainties in loggf values, we assessed solar abundance using a very high-resolution (R~1000000) disk-integrated solar spectrum. These lines were confirmed to be blend-free in the solar spectrum. The line list was further validated by analyzing the metal-poor star HD,218209 (G6V), which is notable for its well-documented and reliable abundance in literature. The abundances were obtained using the equivalent width (EW) method and further refined by applying the spectrum synthesis method. A comparative analysis with the Gaia-ESO line list v.6, provided by the Gaia-ESO collaboration, revealed additional neutral and ionized Fe lines. This extensively refined line list will facilitate precise stellar parameter determinations and accurate abundance analyses of spectra within the PolarBASE spectral library.2025PAREP...2...65Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/other/PARep/2.65CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/other/PARep/2.65https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/other/PARep/2.65http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/other/PARep/2.65https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/other/PARep/2.65https://vizier.iucaa.in/viz-bin/votable?-source=J/other/PARep/2.65http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/other/PARep/2.65GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/other/PARep/2.65/table1Stellar atmospheric parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarTarget namemeta.id;meta.maincharTeffEffective temperatureKphys.temperature.effectiveinte_TeffUncertainty in TeffKstat.error;phys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloate_loggUncertainty in logglog(cm.s**-2)stat.errorfloat[Fe/H]Metallicityphys.abund.Zfloate_[Fe/H]Uncertainty in [Fe/H]stat.error;phys.abund.FefloatVmicMicroturbulent velocitykm/sphys.velocfloate_VmicUncertainty in Vmickm/sstat.errorfloatJ/other/PARep/2.65/table2Elemental abundance ratiosrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSpeciesElement and ionization state (e.g., Fe I, Ti II)phys.atmol.element;phys.atmol.ionizationcharn_Species[*] * for abundances calculated via the spectrum synthesis methodmeta.notechar[X/Fe]*? Abundance ratio [X/Fe] for HD 218209phys.abund;arith.ratiofloatnullablee_[X/Fe]*? Uncertainty in [X/Fe] (HD 218209)stat.error;phys.abundfloatnullableo_[X/Fe]*? Number of lines used in the analysismeta.numberintnullablelogepsSunLogarithmic abundances calculated for the Sunphys.abundfloate_logepsSunUncertainty in logeps(X) for the Sunstat.errorfloato_logepsSunNumber of lines used in the Solar analysismeta.numberintlogeps(X)? Logarithmic abundances for the Sun from Sahin et al., 2023PARep...1...54Sphys.abundfloatnullablee_logeps(X)? Uncertainty in logeps(X) for the Sun from Sahin et al., 2023PARep...1...54Sstat.errorfloatnullableN? Number of lines used from previous work Sahin et al., 2023PARep...1...54Smeta.numberintnullablelogeps(X)ASP09Logarithmic abundances for the Sun from Asplund et al., 2009ARA&A..47..481Aphys.abundfloate_logeps(X)ASP09Uncertainty in logeps(X)_ASP09stat.errorfloatdeltaASP09Difference logarithmic abundance relative to Asplund et al., 2009ARA&A..47..481Aphys.abundfloatlogeps(X)ASP21Logarithmic abundances for the Sun from Asplund et al., 2021A&A...653A.141Aphys.abundfloate_logeps(X)ASP21Uncertainty in logeps(X)_ASP21stat.errorfloatdeltaASP21Difference logarithmic abundance relative to Asplund et al., 2021A&A...653A.141Aphys.abundfloatJ/other/PARep/2.65/tableaSpectral line list with EWs and abundancesRMT? Rowland Multiplet Numbermeta.id;meta.mainintnullableRefReference sources for the adopted loggf value (1)meta.ref;pos.frameintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSpeciesElement and ionization statephys.atmol.element;phys.atmol.ionizationcharlambdaWavelength of the transition0.1nmem.wl;phys.atmol.transitionfloatLEPLower excitation potentialeVphys.atmol.excitation;stat.minfloatloggfOscillator strength or transition probabilityphys.atmol.oscStrengthfloatEW? Equivalent width in the Sun0.1pmspect.line.eqWidthfloatnullablen_EW[s] s for synmeta.notecharlogepsSun? Logarithmic abundances for the Sunphys.abundfloatnullablen_logepsSun[s] s for synmeta.notecharEW*? Equivalent width in the HD 2182090.1pmspect.line.eqWidthfloatnullablen_EW*[s] s for synmeta.notecharlogeps*? Logarithmic abundances for HD 218209phys.abundfloatnullable