J/A+A/668/A168ivo://CDS.VizieR/J/A+A/668/A168doi:10.26093/cds/vizier.36680168CDSCescutti G.Bonifacio P.Caffau E.Monaco L.Franchini M.Lombardo L.,Matas Pinto A.M.Lucertini F.Francois P.Spitoni E.Lallement R.,Sbordone L.Mucciarelli A.Spite M.Hansen C.J.Di Marcantonio P.,Kucinskas A.Dobrovolskas V.Korn A.Valentini M.Magrini L.,Cristallo S.Matteucci F.2024-11-06T20:01:39Z2022-12-19T14:43:00ZCDS support team

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

cds-question@unistra.frmilky-way-galaxygiant-starsspectroscopyvisible-astronomychemical-abundancesIn recent years, Galactic archaeology has become a particularly vibrant field of astronomy, with its main focus set on the oldest stars of our Galaxy. In most cases, these stars have been identified as the most metal-poor. However, the struggle to find these ancient fossils has produced an important bias in the observations - in particular, the intermediate metal-poor stars (-2.5<[Fe/H]<-1.5) have been frequently overlooked. The missing information has consequences for the precise study of the chemical enrichment of our Galaxy, in particular for what concerns neutron capture elements and it will be only partially covered by future multi object spectroscopic surveys such as WEAVE and 4MOST. Measuring at Intermediate Metallicity Neutron Capture Elements (MINCE) is gathering the first high-quality spectra (high signal-to-noise ratio, S/N, and high resolution) for several hundreds of bright and metal-poor stars, mainly located in our Galactic halo. Methods. We compiled our selection mainly on the basis of Gaia data and determined the stellar atmospheres of our sample and the chemical abundances of each star. In this paper, we present the first sample of 59 spectra of 46 stars. We measured the radial velocities and computed the Galactic orbits for all stars. We found that 8 stars belong to the thin disc, 15 to disrupted satellites, and the remaining cannot be associated to the mentioned structures, and we call them halo stars. For 33 of these stars, we provide abundances for the elements up to zinc. We also show the chemical evolution results for eleven chemical elements, based on recent models. Our observational strategy of using multiple telescopes and spectrographs to acquire high S/N and high-resolution spectra for intermediate-metallicity stars has proven to be very efficient, since the present sample was acquired over only about one year of observations. Finally, our target selection strategy, after an initial adjustment, proved satisfactory for our purposes.2022A&A...668A.168Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/668/A168CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/668/A168https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/668/A168http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/668/A168https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/668/A168https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/668/A168http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/668/A168GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/668/A168/abund (Chemical abundances (tables C1-C3))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/668/A168/abund?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/668/A168/abund?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/668/A168/abund?GETtext/xml+votable180.050000true270.947291739.54202780.0055555555555555566/2457 3510 5312 8456 9144 9436 9672 10726 11366 12343 12746 12835 13120 13531 14164 15661 15879 16004 16267 17853 18800 18972 19472 19484 19492 25644 25784 26078 31650 31672 31848 32427 32759https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/668/A168?format=asciiOpticaldefaultJ/A+A/668/A168/abundChemical abundances (tables C1-C3)sigma-ScIILine-to-line scatter for ScIIstat.stdevfloato_ScIINumber of lines used for ScIImeta.numberint[TiI/H]Abundance relative to the Sun for TiIphys.abundfloatsigma-TiILine-to-line scatter for TiIstat.stdevfloato_TiINumber of lines used for TiImeta.numberint[TiII/H]Abundance relative to the Sun for TiIIphys.abundfloatsigma-TiIILine-to-line scatter for TiIIstat.stdevfloato_TiIINumber of lines used for TiIImeta.numberint[VI/H]Abundance relative to the Sun for VIphys.abundfloatsigma-VILine-to-line scatter for VIstat.stdevfloato_VINumber of lines used for VImeta.numberint[CrI/H]Abundance relative to the Sun for CrIphys.abundfloatsigma-CrILine-to-line scatter for CrIstat.stdevfloato_CrINumber of lines used for CrImeta.numberintsigma-NiILine-to-line scatter for NiIstat.stdevfloato_NiINumber of lines used for NiImeta.numberint[CuI/H]? Abundance relative to the Sun for CuIphys.abundfloatnullable[MnI/H]Abundance relative to the Sun for MnIphys.abundfloatsigma-MnILine-to-line scatter for MnIstat.stdevfloato_MnINumber of lines used for MnImeta.numberint[FeI/H]Abundance relative to the Sun for FeIphys.abundfloatsigma-FeILine-to-line scatter for FeIstat.stdevfloato_FeINumber of lines used for FeImeta.numberint[FeII/H]Abundance relative to the Sun for FeIIphys.abundfloatsigma-FeIILine-to-line scatter for FeIIstat.stdevfloato_FeIINumber of lines used for FeIImeta.numberint[CoI/H]Abundance relative to the Sun for CoIphys.abundfloatsigma-CoILine-to-line scatter for CoIstat.stdevfloato_CoINumber of lines used for CoImeta.numberint[CrII/H]Abundance relative to the Sun for CrIIphys.abundfloat[NiI/H]Abundance relative to the Sun for NiIphys.abundfloatsigma-CuILine-to-line scatter for CuIstat.stdevfloato_CuINumber of lines used for CuImeta.numberint[ZnI/H]? Abundance relative to the Sun for ZnIphys.abundfloatnullablesigma-ZnILine-to-line scatter for ZnIstat.stdevfloato_ZnINumber of lines used for ZnImeta.numberint_RAPositions from Simbad (right ascension part)degpos.eq.ra;meta.main_DEPositions from Simbad (declination part)degpos.eq.dec;meta.mainFlag[abc] Instrument flag (G1)meta.code.errorcharo_CaINumber of lines used for CaImeta.numberintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStellar namemeta.id;meta.maincharSimbadNameSimbad column added by the CDSmeta.idcharnullableInstName of the Spectrographmeta.id;instrcharS/NSignal to Noisestat.snrchar[OI/H]? Abundance relative to the Sun for OIphys.abundfloatnullablesigma-OILine-to-line scatter for OIstat.stdevfloato_OINumber of lines used for OImeta.numberint[NaI/H]? Abundance relative to the Sun for NaIphys.abundfloatnullablesigma-NaILine-to-line scatter for NaIstat.stdevfloato_NaINumber of lines used for NaImeta.numberint[MgI/H]Abundance relative to the Sun for MgIphys.abundfloatsigma-MgILine-to-line scatter for MgIstat.stdevfloato_MgINumber of lines used for MgImeta.numberint[AlI/H]? Abundance relative to the Sun for AlIphys.abundfloatnullablesigma-AlILine-to-line scatter for AlIstat.stdevfloato_AlINumber of lines used for AlImeta.numberint[SiI/H]Abundance relative to the Sun for SiIphys.abundfloatsigma-SiILine-to-line scatter for SiIstat.stdevfloato_SiINumber of lines used for SiImeta.numberint[CaI/H]Abundance relative to the Sun for CaIphys.abundfloatsigma-CaILine-to-line scatter for CaIstat.stdevfloat[ScII/H]Abundance relative to the Sun for ScIIphys.abundfloatsigma-CrIILine-to-line scatter for CrIIstat.stdevfloato_CrIINumber of lines used for CrIImeta.numberintJ/A+A/668/A168/linesStellar atmospheres (table B1)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElChemical elementphys.atmol.elementcharZAtomic numberphys.atmol.numberintionIonization statephys.atmol.ionStageintStarStellar namemeta.id;meta.maincharFlag[abc] Instrument flag (G1)meta.code.errorcharlambdaWavelengthnmem.wldoubleloggfloggfphys.absorption.coefffloatElowEnergy of the lower statecm**-1phys.energydouble