J/A+A/635/A114ivo://CDS.VizieR/J/A+A/635/A114doi:10.26093/cds/vizier.36350114CDSHusser T.-O.Latour M.Brinchmann J.Dreizler S.Giesers B.,Goettgens F.Kamann S.Roth M.M.Weilbacher P.M.Wendt M.2021-06-01T08:49:37Z2020-03-18T07:28:36ZCDS support team

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

cds-question@unistra.frglobular-star-clustersgiant-starsmetallicityline-intensitiesThe CaII triplet in the near-infrared at 8498, 8542, and 8662{AA} is visible in stars with spectral types between F and M and can be used to determine their metallicities. We calibrated the relation using average cluster metallicities from literature and MUSE spectra, and extend it below the horizontal branch - a cutoff that has traditionally been made to avoid a non-linear relation - using a quadratic function. In addition to the classic relation based on V-\vhb$ we used calibrations based on absolute magnitude and luminosity and used it for those cluster, for which no HB brightness was available. The obtained relations are then used to calculate metallicities for all the stars in the sample.2020A&A...635A.114Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/635/A114CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/AJ/133/1658 : ACS survey of galactic globular clusters (Sarajedini+, 2007)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/635/A114https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/635/A114http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/635/A114https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/635/A114https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/635/A114http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/635/A114GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/635/A114/musecat (Measured equivalent widths of >30000 red giant branch stars in 25 globular clusters (table 8))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/635/A114/musecat?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/635/A114/musecat?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/635/A114/musecat?GETtext/xml+votable180.050000true6.012736-72.10984320.0055555555555555566/12405 19091 21017 28705 28751 28778 28972-28973 29195 31019 31115 31417 33321 33330 34242 37294 38465 42314 42841 42990 43125 43227 47125 47168 47777 47868 48434https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/635/A114?format=asciidefaultJ/A+A/635/A114/musecatMeasured equivalent widths of >30000 red giant branch stars in 25 globular clusters (table 8)EW2EW of 2nd CaT line from Voigt profile fit0.1nmspect.line.eqWidthdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClusterName of globular cluster (NGC NNNN)meta.id.parentcharIdUnique ID of star within its clustermeta.idintRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainindexedDEJ2000Declination (J2000)degpos.eq.dec;meta.mainindexedEW1EW of 1st CaT line from Voigt profile fit0.1nmspect.line.eqWidthdoublee_EW1Uncertainty for EW of 1st line0.1nmstat.errordoublee_EW2Uncertainty for EW of 2nd line0.1nmstat.errordoubleEW3EW of 3rd CaT line from Voigt profile fit0.1nmspect.line.eqWidthdoublee_EW3Uncertainty for EW of 3rd line0.1nmstat.errordoubleEW1intEW of 1st CaT line from integration0.1nmspect.line.eqWidthdoubleEW2intEW of 2nd CaT line from integration0.1nmspect.line.eqWidthdoubleEW3intEW of 3rd CaT line from integration0.1nmspect.line.eqWidthdoubleREW1? Derived reduced EW from linear relation with stars brighter than HBspect.line.eqWidthdoublenullablee_REW1? Uncertainty for reduced EWstat.errordoublenullable[Fe/H]1? Derived metallicity from linear relation with stars brighter than HBlog(Sun)phys.abund.Zdoublenullablee_[Fe/H]1? Uncertainty for metallicitylog(Sun)stat.error;phys.abund.FedoublenullableREW2? Derived reduced EW from quadratic relation with all RGB starsspect.line.eqWidthdoublenullablee_REW2? Uncertainty for reduced EWstat.errordoublenullable[Fe/H]2? Derived metallicity from quadratic relation with all RGB starslog(Sun)phys.abund.Zdoublenullablee_[Fe/H]2? Uncertainty for metallicitylog(Sun)stat.error;phys.abund.FedoublenullableREW3? Derived reduced EW from calibration based on absolute magnitudespect.line.eqWidthdoublenullablee_REW3? Uncertainty for reduced EWstat.errordoublenullable[Fe/H]3? Derived metallicity from calibration based on absolute magnitudelog(Sun)phys.abund.Zdoublenullablee_[Fe/H]3? Uncertainty for metallicitylog(Sun)stat.error;phys.abund.FedoublenullableREW4? Derived reduced EW from calibration based on luminosityspect.line.eqWidthdoublenullablee_REW4? Uncertainty for reduced EWstat.errordoublenullable[Fe/H]4? Derived metallicity from calibration based on luminositylog(Sun)phys.abund.Zdoublenullablee_[Fe/H]4? Uncertainty for metallicitylog(Sun)stat.error;phys.abund.Fedoublenullable