J/A+A/713/A219ivo://CDS.VizieR/J/A+A/713/A219CDSVitali S.Jofre P.Casamiquela L.Soubiran C.Heiter U.,Aguilera-Gomez C.Barrios-Lopez D.Blanco-Cuaresma S.Escorza A.,Hernandez-Araya I.Signor T.Sinclair-Wentworth H.Worley C.2026-09-18T08:30:13Z2026-09-18T09:29:31ZCDS support team

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

cds-question@unistra.frsurveysf-starschemical-abundancesline-intensitiesvisible-astronomyIn the current era, in which an unprecedented wealth of data are available for the study of the Milky Way, Gaia benchmark stars (GBSs) have become an established reference and calibration sample. Studies of stellar structure and evolution and of the chemical history of our Galaxy generally rely on large spectroscopic surveys and their output catalogs. In this context, deriving precise and accurate stellar parameters and chemical abundances is of paramount importance. This study provides the determination of neutron-capture element abundances and extends the set of chemical abundances available for the third GBS release (GBSv3). Based on the compilation of high-resolution spectra assembled for GBSv3 and consistent with the spectral analysis adopted for the chemical abundances of GBSv3, we used the public iSpec code to derive heavy element abundances. We inferred homogeneous abundances of neutron-capture elements (Y, Zr, Mo, Ba, La, Ce, Pr, Nd, and Eu) across the GBSv3 sample using an in-depth line assessment tailored to different groups identified through a clustering algorithm that accounts for the diversity in stellar parameters and metallicities. This approach addresses key challenges in the spectral analysis of these elements, including the paucity of usable lines, weak line strengths, saturation effects, and sensitivity to atomic data. The assessment yielded reliable measurements, establishing an extended and robust reference scale in good agreement with the literature. This compilation of neutron-capture abundances is based on the GBS sample's robust and accurate atmospheric parameters and the analysis of a large sample of stellar spectra per star, which provides a reliable and homogeneous spectral analysis. It also supports the use of chemical abundances as precise tracers of the Milky Way's star formation history and chemical evolution and constitutes a legacy sample for the calibration of current and future spectroscopic surveys.2026A&A...713A.219Vhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/713/A219CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/682/A145 : Gaia FGK benchmark stars v3 (Soubiran+, 2024)J/A+A/705/A167 : Gaia FGK benchmark stars. Abundances (Casamiquela+, 2026)J/A+A/645/A106 : Atomic data for the Gaia-ESO Survey (Heiter+, 2021)https://www.blancocuaresma.com/s/benchmarkstars :https://gaiabenchmarkstars.com/ : Gaia benchmark stars websitehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/713/A219https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/713/A219http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/713/A219https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/713/A219https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/713/A219http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/713/A219GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/713/A219/stars (List of studied stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/713/A219/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/713/A219/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/713/A219/stars?GETtext/xml+votable180.050000true308.0987083-9.85336110.0055555555555555566/15 137 428 679 684 998 1341 1410 2691 2837 2921 2923 2997 3036 3102 3118 3619 3639 3712 4146 4376 4438 4559 4574 4854 4990 5009 5304 5382 5535 5670 5853 5982 6066 6219 7238 7264 8476 8767 8834 8845 8986 8995 9083 9127 9216 9327 9476 9717 10084 10375 10899 11394 11403 11633 11732 11910 12056 12704 12944 12953 12960 13301 13332-13333 13440 13550 14084 14239 14278 14419 14744 14757 14948 15044 15107 15118 15170 15174 15176 15273 15320 15356 15567 15597 15895 16035 16069 16115 16192 16689 17262 17425 17496 17568 17582 17723 17752 17854 18139 18688 18893 18907 19323 19585 19912 20145 20278 20308 20328 20390 21182 21469 21477 21484 22015 22120 22300 22708 23096 23140 23190 23201 23230 23283 23369 23540 23753 23820 24151 24715 26302 26457 26552 26575 26952 26975 27198 27220 27568 27857 28605 28664 30228 30339 30419 30529 30665 30878 30965 31416 31433 31576 31784 32192 32561 32645 32754 32994 33281 33377 33874 34051 34169 34263 34730 35025 35118 35185 35382 35415 35532 35602 35673 36035 36433 36693 36697 36723 36803 37507 38072 38216 39026 39340 40618 40692 41763 42081 42248 44284 44542 45564 45668 46176 48519 49060https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/713/A219?format=asciiOpticaldefaultJ/A+A/713/A219/starsList of studied starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSimbadNameSimbad column added by the CDSmeta.idcharnullableNameStar ID (HIP identifier) or Sunmeta.id;meta.maincharRAJ2000? Simbad right ascension (J2000)pos.eq.ra;meta.mainnullableDEJ2000? Simbad declination (J2000)pos.eq.dec;meta.mainnullableJ/A+A/713/A219/table1Final element abundances for the entire GBSv3 samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar ID (HIP identifier) or Sunmeta.id;meta.maincharClusterGroupStellar group from clustering algorithmmeta.idchar[Fe/H]Iron abundance [FeI/H]phys.abunddoubleElementElement name and ionization stagemeta.id;phys.atmol.ionStage;phys.atmol.ionizationchar[X/Fe]Abundance ratio [X/Fe] (1)phys.abund;arith.ratiodoublee_[X/Fe]Abundance error on [X/Fe]stat.error;phys.abunddoubleJ/A+A/713/A219/table2Atomic line parameters for the n-capture elements analyzedrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLineNameLine identifier (element_wavelength) (1)meta.id;spect.linecharWavePeakCentral wavelength of the spectral linenmem.wl.centraldoubleElementElement symbolphys.atmol.elementcharSpecies[39/63] Atomic number of the elementphys.atmol.elementintIsotope[1/2] Ionization stage (1=neutral, 2=ionized)meta.codeintLowerStateeVLower excitation potential of the transitioneVphys.atmol.excitation;stat.minfloatloggfOscillator strength of the line (log gf)spect.line.intensityfloatJ/A+A/713/A219/table3Line-by-line abundances per spectrum and instrumentrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar ID (HIP identifier) or Sun (1)meta.id;meta.maincharSpecIDSpectrum origin (STAR_INST)meta.idcharAbundanceAbsolute abundance A(X) measured for this line in this spectrumphys.abunddoubleElementElement symbolphys.atmol.elementcharIon[1/2] Ionization stage (1=neutral, 2=ionized)phys.atmol.ionStageintWavePeakCentral wavelength of the spectral linenmem.wl.centralfloatJ/A+A/713/A219/table4Equivalent widths per spectrum and lineEWEquivalent width measured for this line in this spectrum0.1nmspect.line.eqWidthdoubleElementElement symbolphys.atmol.elementcharIon[1/2] Ionization stage (1=neutral, 2=ionized)phys.atmol.ionStageintWavePeakCentral wavelength of the spectral linenmem.wl.centralfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar ID (HIP identifier) or Sun (1)meta.id;meta.maincharSpecIDSpectrum origin (STAR_INST)meta.idcharJ/A+A/713/A219/table5Recommended abundances per starrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar ID (HIP identifier)meta.id;meta.mainchargrStellar group from clustering algorithm (roman numeral, I-X)meta.idchar[Fe/H]Iron abundance [FeI/H]phys.abundfloat[YII/H]? Abundance [YII/H] (1)phys.abundfloatnullablee_[YII/H]? Abundance error on [YII/H]stat.error;phys.abundfloatnullable[ZrI/H]? Abundance [ZrI/H] (1)phys.abundfloatnullablee_[ZrI/H]? Abundance error on [ZrI/H]stat.error;phys.abundfloatnullable[ZrII/H]? Abundance [ZrII/H] (1)phys.abundfloatnullablee_[ZrII/H]? Abundance error on [ZrII/H]stat.error;phys.abundfloatnullable[MoI/H]? Abundance [MoI/H] (1)phys.abundfloatnullablee_[MoI/H]? Abundance error on [MoI/H]stat.error;phys.abundfloatnullable[BaII/H]? Abundance [BaII/H] (1)phys.abundfloatnullablee_[BaII/H]? Abundance error on [BaII/H]stat.error;phys.abundfloatnullable[LaII/H]? Abundance [LaII/H] (1)phys.abundfloatnullablee_[LaII/H]? Abundance error on [LaII/H]stat.error;phys.abundfloatnullable[CeII/H]? Abundance [CeII/H] (1)phys.abundfloatnullablee_[CeII/H]? Abundance error on [CeII/H]stat.error;phys.abundfloatnullable[PrII/H]? Abundance [PrII/H] (1)phys.abundfloatnullablee_[PrII/H]? Abundance error on [PrII/H]stat.error;phys.abundfloatnullable[NdII/H]? Abundance [NdII/H] (1)phys.abundfloatnullablee_[NdII/H]? Abundance error on [NdII/H]stat.error;phys.abundfloatnullable[EuII/H]? Abundance [EuII/H] (1)phys.abundfloatnullablee_[EuII/H]? Abundance error on [EuII/H]stat.error;phys.abundfloatnullable