J/A+A/592/A70ivo://CDS.VizieR/J/A+A/592/A70doi:10.26093/cds/vizier.35920070CDSHawkins K.Jofre P.Heiter U.Soubiran C.Blanco-Cuaresma S.,Casagrande L.Gilmore G.Lind K.Magrini L.Masseron T.Pancino E.,Randich S.Worley C.C.2018-08-29T06:47:17Z2016-07-28T08:03:34ZCDS support team

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

cds-question@unistra.frf-starsmetallicityWe have entered an era of large spectroscopic surveys in which we can measure, through automated pipelines, the atmospheric parameters and chemical abundances for large numbers of stars. Calibrating these survey pipelines using a set of "benchmark stars" in order to evaluate the accuracy and precision of the provided parameters and abundances is of utmost importance. The recent proposed set of Gaia FGK benchmark stars has up to five metal-poor stars but no recommended stars within -2.0<[Fe/H]<-1.0dex. However, this metallicity regime is critical to calibrate properly. In this paper, we aim to add candidate Gaia benchmark stars inside of this metal-poor gap. We began with a sample of 21 metal-poor stars which was reduced to 10 stars by requiring accurate photometry and parallaxes, and high-resolution archival spectra. The procedure used to determine the stellar parameters was similar to the previous works in this series for consistency. The difference was to homogeneously determine the angular diameter and effective temperature (Teff) of all of our stars using the Infrared Flux Method utilizing multi-band photometry. The surface gravity (logg) was determined through fitting stellar evolutionary tracks. The [Fe/H] was determined using four different spectroscopic methods fixing the Teff and logg from the values determined independent of spectroscopy.2016A&A...592A..70Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/592/A70CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toIII/281 : Gaia FGK benchmark stars v2.1 (Jofre+, 2018)J/A+A/564/A133 : Gaia FGK benchmark stars: metallicity (Jofre+, 2014)J/A+A/566/A98 : Gaia FGK benchmark Stars - Library (Blanco-Cuaresma+, 2014)J/A+A/582/A81 : Gaia FGK benchmark stars: abundances (Jofre+, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/592/A70https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/592/A70http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/592/A70https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/592/A70https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/592/A70http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/592/A70GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/592/A70/sources (General information on metal-poor benchmark candidates selected (from table 1 of the paper))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/592/A70/sources?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/592/A70/sources?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/592/A70/sources?GETtext/xml+votable180.050000true325.98827.390.0055555555555555566/12704 12793 16115 17099 23015 27857 38072 38216 44653 48731https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/592/A70?format=asciidefaultJ/A+A/592/A70/sourcesGeneral information on metal-poor benchmark candidates selected (from table 1 of the paper)StarStar namemeta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainTeffEffective temperature (1)Kphys.temperature.effectiveinte_Teffrms uncertainty on Teff (1)Kstat.error;phys.temperature.effectiveinto_TeffNumber of references in PASTEL database for Teffmeta.numberintloggSurface gravity (1)log(cm.s**-2)phys.gravityfloate_loggrms uncertainty on logg (1)log(cm.s**-2)stat.errorfloato_loggNumber of references in PASTEL database for loggmeta.numberint[Fe/H]Metallicity (1)phys.abund.Zfloate_[Fe/H]rms uncertainty on [Fe/H] (1)stat.error;phys.abund.Fefloato_[Fe/H]Number of references in PASTEL database for [Fe/H]meta.numberintTableName of the table with Fe abundance measurementsmeta.id;phys.abund.Fe;meta.tablecharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/A+A/592/A70/tablea1BD+26 4251 Fe abundance measurements for each line and noderecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementElement and Ion statephys.atmol.elementcharlambdaWavelength of line used in the abundance determination0.1nmem.wl;spect.linefloat<EW>Mean Equivalent width from all nodes0.1pmspect.line.eqWidth;stat.meanfloat<A>Mean Fe abundance derived for that line across all nodesphys.abund.Fe;stat.meanfloatNLTE? NLTE correction for that line (1)arith.factorfloatnullableEW(EPI)? Equivalent width obtained by the EPINARBO method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(BOL)? Equivalent width obtained by the Bologna method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(ULB)? Equivalent width obtained by the ULB method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(iSPEC)? Equivalent width obtained by the iSPEC method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableA(EPI)? abundance obtained by the EPINARBO method (2)phys.abund.FefloatnullableA(BOL)? abundance obtained by the Bologna method (2)phys.abund.FefloatnullableA(ULB)? abundance obtained by the ULB method (2)phys.abund.FefloatnullableA(iSPEC)? abundance obtained by the iSPEC method (2)phys.abund.FefloatnullableJ/A+A/592/A70/tablea2HD 102200 Fe abundance measurements for each line and noderecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementElement and Ion statephys.atmol.elementcharlambdaWavelength of line used in the abundance determination0.1nmem.wl;spect.linefloat<EW>Mean Equivalent width from all nodes0.1pmspect.line.eqWidth;stat.meanfloat<A>Mean Fe abundance derived for that line across all nodesphys.abund.Fe;stat.meanfloatNLTE? NLTE correction for that line (1)arith.factorfloatnullableEW(EPI)? Equivalent width obtained by the EPINARBO method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(BOL)? Equivalent width obtained by the Bologna method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(ULB)? Equivalent width obtained by the ULB method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(iSPEC)? Equivalent width obtained by the iSPEC method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableA(EPI)? abundance obtained by the EPINARBO method (2)phys.abund.FefloatnullableA(BOL)? abundance obtained by the Bologna method (2)phys.abund.FefloatnullableA(ULB)? abundance obtained by the ULB method (2)phys.abund.FefloatnullableA(iSPEC)? abundance obtained by the iSPEC method (2)phys.abund.FefloatnullableJ/A+A/592/A70/tablea3HD 106038 Fe abundance measurements for each line and noderecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementElement and Ion statephys.atmol.elementcharlambdaWavelength of line used in the abundance determination0.1nmem.wl;spect.linefloat<EW>Mean Equivalent width from all nodes0.1pmspect.line.eqWidth;stat.meanfloat<A>Mean Fe abundance derived for that line across all nodesphys.abund.Fe;stat.meanfloatNLTE? NLTE correction for that line (1)arith.factorfloatnullableEW(EPI)? Equivalent width obtained by the EPINARBO method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(BOL)? Equivalent width obtained by the Bologna method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(ULB)? Equivalent width obtained by the ULB method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(iSPEC)? Equivalent width obtained by the iSPEC method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableA(EPI)? abundance obtained by the EPINARBO method (2)phys.abund.FefloatnullableA(BOL)? abundance obtained by the Bologna method (2)phys.abund.FefloatnullableA(ULB)? abundance obtained by the ULB method (2)phys.abund.FefloatnullableA(iSPEC)? abundance obtained by the iSPEC method (2)phys.abund.FefloatnullableJ/A+A/592/A70/tablea4HD 126681 Fe abundance measurements for each line and noderecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementElement and Ion statephys.atmol.elementcharlambdaWavelength of line used in the abundance determination0.1nmem.wl;spect.linefloat<EW>Mean Equivalent width from all nodes0.1pmspect.line.eqWidth;stat.meanfloat<A>Mean Fe abundance derived for that line across all nodesphys.abund.Fe;stat.meanfloatNLTE? NLTE correction for that line (1)arith.factorfloatnullableEW(EPI)? Equivalent width obtained by the EPINARBO method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(BOL)? Equivalent width obtained by the Bologna method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(ULB)? Equivalent width obtained by the ULB method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(iSPEC)? Equivalent width obtained by the iSPEC method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableA(EPI)? abundance obtained by the EPINARBO method (2)phys.abund.FefloatnullableA(BOL)? abundance obtained by the Bologna method (2)phys.abund.FefloatnullableA(ULB)? abundance obtained by the ULB method (2)phys.abund.FefloatnullableA(iSPEC)? abundance obtained by the iSPEC method (2)phys.abund.FefloatnullableJ/A+A/592/A70/tablea5HD 175305 Fe abundance measurements for each line and node<EW>Mean Equivalent width from all nodes0.1pmspect.line.eqWidth;stat.meanfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementElement and Ion statephys.atmol.elementcharlambdaWavelength of line used in the abundance determination0.1nmem.wl;spect.linefloat<A>Mean Fe abundance derived for that line across all nodesphys.abund.Fe;stat.meanfloatNLTE? NLTE correction for that line (1)arith.factorfloatnullableEW(EPI)? Equivalent width obtained by the EPINARBO method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(BOL)? Equivalent width obtained by the Bologna method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(ULB)? Equivalent width obtained by the ULB method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(iSPEC)? Equivalent width obtained by the iSPEC method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableA(EPI)? abundance obtained by the EPINARBO method (2)phys.abund.FefloatnullableA(BOL)? abundance obtained by the Bologna method (2)phys.abund.FefloatnullableA(ULB)? abundance obtained by the ULB method (2)phys.abund.FefloatnullableA(iSPEC)? abundance obtained by the iSPEC method (2)phys.abund.FefloatnullableJ/A+A/592/A70/tablea6HD 196892 Fe abundance measurements for each line and noderecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementElement and Ion statephys.atmol.elementcharlambdaWavelength of line used in the abundance determination0.1nmem.wl;spect.linefloat<EW>Mean Equivalent width from all nodes0.1pmspect.line.eqWidth;stat.meanfloat<A>Mean Fe abundance derived for that line across all nodesphys.abund.Fe;stat.meanfloatNLTE? NLTE correction for that line (1)arith.factorfloatnullableEW(EPI)? Equivalent width obtained by the EPINARBO method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(BOL)? Equivalent width obtained by the Bologna method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(ULB)? Equivalent width obtained by the ULB method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(iSPEC)? Equivalent width obtained by the iSPEC method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableA(EPI)? abundance obtained by the EPINARBO method (2)phys.abund.FefloatnullableA(BOL)? abundance obtained by the Bologna method (2)phys.abund.FefloatnullableA(ULB)? abundance obtained by the ULB method (2)phys.abund.FefloatnullableA(iSPEC)? abundance obtained by the iSPEC method (2)phys.abund.FefloatnullableJ/A+A/592/A70/tablea7HD 201891 Fe abundance measurements for each line and noderecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementElement and Ion statephys.atmol.elementcharlambdaWavelength of line used in the abundance determination0.1nmem.wl;spect.linefloat<EW>Mean Equivalent width from all nodes0.1pmspect.line.eqWidth;stat.meanfloat<A>Mean Fe abundance derived for that line across all nodesphys.abund.Fe;stat.meanfloatNLTE? NLTE correction for that line (1)arith.factorfloatnullableEW(EPI)? Equivalent width obtained by the EPINARBO method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(BOL)? Equivalent width obtained by the Bologna method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(ULB)? Equivalent width obtained by the ULB method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(iSPEC)? Equivalent width obtained by the iSPEC method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableA(EPI)? abundance obtained by the EPINARBO method (2)phys.abund.FefloatnullableA(BOL)? abundance obtained by the Bologna method (2)phys.abund.FefloatnullableA(ULB)? abundance obtained by the ULB method (2)phys.abund.FefloatnullableA(iSPEC)? abundance obtained by the iSPEC method (2)phys.abund.FefloatnullableJ/A+A/592/A70/tablea8HD 218857 Fe abundance measurements for each line and noderecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementElement and Ion statephys.atmol.elementcharlambdaWavelength of line used in the abundance determination0.1nmem.wl;spect.linefloat<EW>Mean Equivalent width from all nodes0.1pmspect.line.eqWidth;stat.meanfloat<A>Mean Fe abundance derived for that line across all nodesphys.abund.Fe;stat.meanfloatNLTE? NLTE correction for that line (1)arith.factorfloatnullableEW(EPI)? Equivalent width obtained by the EPINARBO method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(BOL)? Equivalent width obtained by the Bologna method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(ULB)? Equivalent width obtained by the ULB method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(iSPEC)? Equivalent width obtained by the iSPEC method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableA(EPI)? abundance obtained by the EPINARBO method (2)phys.abund.FefloatnullableA(BOL)? abundance obtained by the Bologna method (2)phys.abund.FefloatnullableA(ULB)? abundance obtained by the ULB method (2)phys.abund.FefloatnullableA(iSPEC)? abundance obtained by the iSPEC method (2)phys.abund.FefloatnullableJ/A+A/592/A70/tablea9HD 241253 Fe abundance measurements for each line and noderecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementElement and Ion statephys.atmol.elementcharlambdaWavelength of line used in the abundance determination0.1nmem.wl;spect.linefloat<EW>Mean Equivalent width from all nodes0.1pmspect.line.eqWidth;stat.meanfloat<A>Mean Fe abundance derived for that line across all nodesphys.abund.Fe;stat.meanfloatNLTE? NLTE correction for that line (1)arith.factorfloatnullableEW(EPI)? Equivalent width obtained by the EPINARBO method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(BOL)? Equivalent width obtained by the Bologna method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(ULB)? Equivalent width obtained by the ULB method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(iSPEC)? Equivalent width obtained by the iSPEC method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableA(EPI)? abundance obtained by the EPINARBO method (2)phys.abund.FefloatnullableA(BOL)? abundance obtained by the Bologna method (2)phys.abund.FefloatnullableA(ULB)? abundance obtained by the ULB method (2)phys.abund.FefloatnullableA(iSPEC)? abundance obtained by the iSPEC method (2)phys.abund.FefloatnullableJ/A+A/592/A70/tablea10HD 298986 Fe abundance measurements for each line and noderecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementElement and Ion statephys.atmol.elementcharlambdaWavelength of line used in the abundance determination0.1nmem.wl;spect.linefloat<EW>Mean Equivalent width from all nodes0.1pmspect.line.eqWidth;stat.meanfloat<A>Mean Fe abundance derived for that line across all nodesphys.abund.Fe;stat.meanfloatNLTE? NLTE correction for that line (1)arith.factorfloatnullableEW(EPI)? Equivalent width obtained by the EPINARBO method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(BOL)? Equivalent width obtained by the Bologna method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(ULB)? Equivalent width obtained by the ULB method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableEW(iSPEC)? Equivalent width obtained by the iSPEC method (2)0.1pmspect.line.eqWidth;meta.modelledfloatnullableA(EPI)? abundance obtained by the EPINARBO method (2)phys.abund.FefloatnullableA(BOL)? abundance obtained by the Bologna method (2)phys.abund.FefloatnullableA(ULB)? abundance obtained by the ULB method (2)phys.abund.FefloatnullableA(iSPEC)? abundance obtained by the iSPEC method (2)phys.abund.Fefloatnullable