J/A+A/651/A20ivo://CDS.VizieR/J/A+A/651/A20doi:10.26093/cds/vizier.36510020CDSCaffau E.Bonifacio P.Korotin S.A.Francois P.Lallement R.,Matas Pinto A.M.Di Matteo P.Steffen M.Mucciarelli A.Katz D.,Haywood M.Chemin L.Sartoretti P.Sbordone L.Andrievsky S.M.,Kovtyukh V.V.Spite M.Spite F.Panuzzo P.Royer F.Thevenin F.,Ludwig H.-G.Marchal O.Plum G.2023-01-11T14:13:30Z2021-07-02T08:28:16ZCDS support team

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

cds-question@unistra.frmilky-way-galaxylate-type-starschemical-abundancesThe Radial Velocity Spectrometer (RVS) on board the Gaia satellite is not provided with a wavelength calibration lamp. It uses its observations of stars with known radial velocity to derive the dispersion relation. To derive an accurate radial velocity calibration, a precise knowledge of the line spread function (LSF) of the RVS is necessary. Good-quality ground-based observations in the wavelength range of the RVS are highly desired to determine the LSF. Several radial velocity standard stars are available to the Gaia community. The highest possible number of calibrators will surely allow us to improve the accuracy of the radial velocity. Because the LSF may vary across the focal plane of the RVS, a large number of high-quality spectra for the LSF calibration may allow us to better sample the properties of the focal plane. We selected a sample of stars to be observed with UVES at the Very Large Telescope, in a setting including the wavelength range of RVS, that are bright enough to allow obtaining high-quality spectra in a short time. We also selected stars that lack chemical investigation in order to increase the sample of bright, close by stars with a complete chemical inventory. We here present the chemical analysis of the first sample of 80 evolved stars. The quality of the spectra is very good, therefore we were able to derive abundances for 20 elements. The metallicity range spanned by the sample is about 1dex, from slightly metal-poor to solar metallicity. We derived the Rb abundance for all stars and investigated departures from local thermodynamical equilibrium (NLTE) in the formation of its lines. The sample of spectra is of good quality, which is useful for a Gaia radial velocity calibration. The Rb NLTE effects in this stellar parameters range are small but sometimes non-negligible, especially for spectra of this good quality.2021A&A...651A..20Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/651/A20CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/350 : Gaia EDR3 (Gaia Collaboration, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/651/A20https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/651/A20http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/651/A20https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/651/A20https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/651/A20http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/651/A20GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/651/A20/tableb3 (Detailed chemical abundances)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/651/A20/tableb3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/651/A20/tableb3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/651/A20/tableb3?GETtext/xml+votable180.050000true19.92765-33.721140.0055555555555555566/8331 12291 20592 20640 20661 20895 21102 21126 21130 21227 21389 21772 21793 22186 22595 22598 22653 22788 22791 22932 22951 22980 23705 24636 24738 24802 24854 24874 25087 25287 25500 25503 26895 34142 34295 34405 34445 34580 35631 37549 37637 37756 37912 37962 38029 38034 38203 38217 38256 38259 38293 38390 38464 38506 38830 38847 39240 39428 39586 40030 40205 40227 40546 40559 40671 41717 41770 41854 41947 41949 42550 43165 43210 43246 43588 43617 43716 43828 45887 46410https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/651/A20?format=asciidefaultJ/A+A/651/A20/tableb3Detailed chemical abundanceso_Ca? Number of Ca linesmeta.numberintnullablee_A(TiII)? Uncertainty on A(Ti) derived from TiII linesphys.abunddoublenullableA(V)A(V) abundance (1)phys.abunddoublee_A(V)Uncertainty on A(V)phys.abunddoubleo_V? Number of VI linesmeta.numberintnullableA(CrI)A(Cr) abundance (1)phys.abunddoublee_A(CrI)Uncertainty on A(Cr)phys.abunddoubleo_CrI? Number of CrI linesmeta.numberintnullableA(Mn)A(Mn) abundance (1)phys.abunddoublee_A(Mn)Uncertainty on A(Mnphys.abunddoubleo_Mn? Number of MnI linesmeta.numberintnullableA(Co)A(Co) abundance (1)phys.abunddoublee_A(Co)Uncertainty on A(Co)phys.abunddoubleo_Co? Number of CoI linesmeta.numberintnullableA(Ni)A(Ni) abundance (1)phys.abunddoublee_A(Ni)Uncertainty on A(Ni)phys.abunddoubleo_Ni? Number of NiI linesmeta.numberintnullableA(Rb)NLTEA(Rb) abundance under NLTE assumption (1)phys.abunddoubleA(Rb)LTEA(Rb) abundance under LTE assumption (1)phys.abunddoubleA(Sr)A(Sr) abundance (1)phys.abunddoubleA(Y)A(Y) abundance (1)phys.abunddoubleA(Ba)A(Ba) abundance (1)phys.abunddoubleA(Eu)A(Eu) abundance (1)phys.abunddoubleRAodegObserved right ascensiondegpos.eq.raDEodegObserved declinationdegpos.eq.decRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainTeffEffective temperatureKphys.temperature.effectiveintSimbadSimbad column added by the CDSmeta.ref.urlcharDEJ2000Declination (J2000)degpos.eq.dec;meta.mainGaiaEDR3GaiaEDR3 source_idmeta.idRVSStellar identifier (RVSNNN)meta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogglog surface gravitylog(cm.s**-2)phys.gravityfloatxiMicroturbulence velocitykm/sphys.veloc.microTurbdoubleA(FeI)A(Fe) derived from FeI linesphys.abunddoublee_A(FeI)Uncertainty on A(Fe) derived from FeI linesphys.abunddoubleo_FeI? Number of FeI linesmeta.numberintnullableA(FeII)A(Fe) derived from FeII lines (1)phys.abunddoublee_A(FeII)Uncertainty on A(Fe) derived from FeII linesphys.abunddoubleo_FeII? Number of FeII lines (1)meta.numberintnullableA(C)A(C) abundance (1)phys.abunddoubleA(O)A(O) abundance (1)phys.abunddoubleA(Na)A(Na) abundance (1)phys.abunddoublee_A(Na)? Uncertainty on A(Na)phys.abunddoublenullableo_Na? Number of Na lines (1)meta.numberintnullableA(Mg)A(Mg) abundance (1)phys.abunddoublee_A(Mg)? Uncertainty on A(Mg)phys.abunddoublenullableo_Mg? Number of MgI lines (1)meta.numberintnullableA(Al)A(Al) abundance (1)phys.abunddoublee_A(Al)Uncertainty on A(Al)phys.abunddoubleo_Al? Number of AlI lines (1)meta.numberintnullablee_A(Ca)Uncertainty on A(Ca)phys.abunddoubleA(Si)A(Si) abundance (1)phys.abunddoublee_A(Si)Uncertainty on A(Si)phys.abunddoubleo_si? Number of SiI linesmeta.numberintnullableA(S)? A(S) abundance (1)phys.abunddoublenullablee_A(S)? Uncertainty on A(S)phys.abunddoublenullableA(Ca)A(Ca) abundance (1)phys.abunddoubleA(ScI)A(Sc) abundance derived from ScI lines (1)phys.abunddoublee_A(ScI)? Uncertainty on A(Sc) derived from ScI linesphys.abunddoublenullableo_ScI? Number of ScI linesmeta.numberintnullableA(ScII)A(Sc) abundance derived from ScII lines (1)phys.abunddoublee_A(ScII)? Uncertainty on A(Sc) derived from ScII linesphys.abunddoublenullableo_ScII? Number of ScII linesmeta.numberintnullableA(TiI)A(Ti) abundance derived from TiI lines (1)phys.abunddoublee_A(TiI)Uncertainty on A(Ti) derived from TiI linesphys.abunddoubleo_TiI? Number of TiI linesmeta.numberintnullableA(TiII)A(Ti) derived from TiII lines (1)phys.abunddoubleo_TiII? Number of TiII linesmeta.numberintnullableJ/A+A/651/A20/tablecLines used in the chemical investigation for each element and for each star in the samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElElement (1)phys.atmol.elementcharZElement numberphys.atmol.numberintIon[0/1]phys.atmol.ionStageintRVSStar name (RVSNNN)meta.id;meta.maincharlambdaWavelengthnmem.wldoubleloggfOscillator strengthphys.atmol.oscStrengthfloatElowLowerEnergycm**-1phys.energy;phys.atmol.leveldouble