J/A+A/713/A60ivo://CDS.VizieR/J/A+A/713/A60CDSAlazzawi J.M.K.Caffau E.Bonifacio P.Caliskan S.Monaco L.,Sbordone L.Lombardo L.2026-09-07T07:44:42Z2026-09-07T08:42:14ZCDS support team

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

cds-question@unistra.frmilky-way-galaxychemically-peculiar-starshigh-velocity-starschemical-abundancesvisible-astronomyOld, metal-poor stars are perfect tracers of the formation of the Milky Way. The combination of chemical and kinematic investigations into them provides an insight into accretion episodes in the past history of our Galaxy. We present here a detailed chemical abundance analysis of 16 metal-poor stars, selected from the RAVE survey, which are characterised by a high radial velocity. We derived stellar parameters from Gaia photometry and parallaxes. Using high-resolution spectra obtained with UVES at the ESO-VLT, we determined elemental abundances for alpha-, iron-peak, and neutron-capture elements using the MYGISFOS pipeline. Departures from local thermodynamic equilibrium, where available, were investigated. We used the SPInS bayesian inference pipeline to derive ages for all the stars. Actions and other dynamical quantities were computed using the galpy pipeline applying the Galactic potential MWPotential2014, in order to classify the stars kinematically. The stars span a wide metallicity range (-1.2<~[Fe/H]<~-2.9) and exhibit kinematic properties consistent with the outer halo population. Star C0213360-505024, [Fe/H]=-1.4, appears to have an age of 1.3Gyr and a mass of 1.6M_{sun}_. Based also on its kinematics and line broadening, which we attribute to stellar rotation, we argue that this star is young and not an evolved blue straggler. The available evidence points towards an accreted origin for this star and we speculate about its possible progenitor. The other 15 stars have ages compatible with an old population.2026A&A...713A..60Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/713/A60CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/713/A60https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/713/A60http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/713/A60https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/713/A60https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/713/A60http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/713/A60GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/713/A60/stars (List of studied stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/713/A60/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/713/A60/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/713/A60/stars?GETtext/xml+votable180.050000true33.400125-50.84013890.0055555555555555566/24748 26164 35079 35479 35513 38874 40280 43848 43913 43915 44017 44453 44518 45448 45727 46389https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/713/A60?format=asciiOpticaldefaultJ/A+A/713/A60/starsList of studied starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar identifier, as used in the papermeta.id;meta.maincharRAJ2000Simbad right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Simbad declination (J2000)pos.eq.dec;meta.mainFileNameName of the table with linelist of the star in subdirectory linelistmeta.id;meta.tablecharSNameSimbad namemeta.idcharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/A+A/713/A60/abundStellar parameters and abundances for every element/ion measuredA(CaI)Mean abundance log(N(CaI)/N(H))+12phys.abundfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar identifier, as used in the papermeta.id;meta.maincharTeffAdopted effective temperatureKphys.temperature.effectiveintloggAdopted surface gravitylog(cm.s**-2)phys.gravityfloatvturbMicroturbulent velocity, xikm/sphys.velocfloat[Fe/H]Derived metallicity from FeI linesphys.abundfloato_O? Number of individual spectral lines used to derive the abundance of [OI] forbidden linemeta.numberintnullableA(O)? Mean abundance log(N(O)/N(H))+12phys.abundfloatnullable[O/H]? Abundance relative to the Sun, A(O)-A(O)_{sun}_phys.abundfloatnullables_O? Line-to-line scatter (standard deviation) of A(O) over the number of lines used (1)phys.atmol.numberfloatnullableo_NaI? Number of individual spectral lines used to derive the abundance of NaImeta.numberintnullableA(NaI)? Mean abundance log(N(NaI)/N(H))+12phys.abundfloatnullable[NaI/H]? Abundance relative to the Sun, A(NaI)-A(NaI)_{sun}_phys.abundfloatnullables_NaI? Line-to-line scatter (standard deviation) of A(NaI) over the number of lines used (1)phys.atmol.numberfloatnullableo_MgINumber of individual spectral lines used to derive the abundance of MgImeta.numberintA(MgI)Mean abundance log(N(MgI)/N(H))+12phys.abundfloat[MgI/H]Abundance relative to the Sun, A(MgI)-A(MgI)_{sun}_phys.abundfloats_MgI? Line-to-line scatter (standard deviation) of A(MgI) over the number of lines used (1)phys.atmol.numberfloatnullableo_AlI? Number of individual spectral lines used to derive the abundance of AlImeta.numberintnullableA(AlI)? Mean abundance log(N(AlI)/N(H))+12phys.abundfloatnullable[AlI/H]? Abundance relative to the Sun, A(AlI)-A(AlI)_{sun}_phys.abundfloatnullables_AlI? Line-to-line scatter (standard deviation) of A(AlI) over the number of lines used (1)phys.atmol.numberfloatnullableo_SiINumber of individual spectral lines used to derive the abundance of SiImeta.numberintA(SiI)Mean abundance log(N(SiI)/N(H))+12phys.abundfloat[SiI/H]Abundance relative to the Sun, A(SiI)-A(SiI)_{sun}_phys.abundfloats_SiILine-to-line scatter (standard deviation) of A(SiI) over the number of lines used (1)phys.atmol.numberfloato_CaINumber of individual spectral lines used to derive the abundance of CaImeta.numberint[CaI/H]Abundance relative to the Sun, A(CaI)-A(CaI)_{sun}_phys.abundfloats_CaILine-to-line scatter (standard deviation) of A(CaI) over the number of lines used (1)phys.atmol.numberfloato_ScIINumber of individual spectral lines used to derive the abundance of ScIImeta.numberintA(ScII)Mean abundance log(N(ScII)/N(H))+12phys.abundfloat[ScII/H]Abundance relative to the Sun, A(ScII)-A(ScII)_{sun}_phys.abundfloats_ScIILine-to-line scatter (standard deviation) of A(ScII) over the number of lines used (1)phys.atmol.numberfloato_TiINumber of individual spectral lines used to derive the abundance of TiImeta.numberintA(TiI)Mean abundance log(N(TiI)/N(H))+12phys.abundfloat[TiI/H]Abundance relative to the Sun, A(TiI)-A(TiI)_{sun}_phys.abundfloats_TiILine-to-line scatter (standard deviation) of A(TiI) over the number of lines used (1)phys.atmol.numberfloato_TiIINumber of individual spectral lines used to derive the abundance of TiIImeta.numberintA(TiII)Mean abundance log(N(TiII)/N(H))+12phys.abundfloat[TiII/H]Abundance relative to the Sun, A(TiII)-A(TiII)_{sun}_phys.abundfloats_TiIILine-to-line scatter (standard deviation) of A(TiII) over the number of lines used (1)phys.atmol.numberfloato_VINumber of individual spectral lines used to derive the abundance of VImeta.numberintA(VI)Mean abundance log(N(VI)/N(H))+12phys.abundfloat[VI/H]Abundance relative to the Sun, A(VI)-A(VI)_{sun}_phys.abundfloats_VILine-to-line scatter (standard deviation) of A(VI) over the number of lines used (1)phys.atmol.numberfloato_CrINumber of individual spectral lines used to derive the abundance of CrImeta.numberintA(CrI)Mean abundance log(N(CrI)/N(H))+12phys.abundfloat[CrI/H]Abundance relative to the Sun, A(CrI)-A(CrI)_{sun}_phys.abundfloats_CrILine-to-line scatter (standard deviation) of A(CrI) over the number of lines used (1)phys.atmol.numberfloato_CrIINumber of individual spectral lines used to derive the abundance of CrIImeta.numberintA(CrII)Mean abundance log(N(CrII)/N(H))+12phys.abundfloat[CrII/H]Abundance relative to the Sun, A(CrII)-A(CrII)_{sun}_phys.abundfloats_CrII? Line-to-line scatter (standard deviation) of A(CrII) over the number of lines used (1)phys.atmol.numberfloatnullableo_MnINumber of individual spectral lines used to derive the abundance of MnImeta.numberintA(MnI)Mean abundance log(N(MnI)/N(H))+12phys.abundfloat[MnI/H]Abundance relative to the Sun, A(MnI)-A(MnI)_{sun}_phys.abundfloats_MnILine-to-line scatter (standard deviation) of A(MnI) over the number of lines used (1)phys.atmol.numberfloato_FeIINumber of individual spectral lines used to derive the abundance of FeIImeta.numberintA(FeII)Mean abundance log(N(FeII)/N(H))+12phys.abundfloat[FeII/H]Abundance relative to the Sun, A(FeII)-A(FeII)_{sun}_phys.abundfloats_FeIILine-to-line scatter (standard deviation) of A(FeII) over the number of lines used (1)phys.atmol.numberfloato_CoINumber of individual spectral lines used to derive the abundance of CoImeta.numberintA(CoI)Mean abundance log(N(CoI)/N(H))+12phys.abundfloat[CoI/H]Abundance relative to the Sun, A(CoI)-A(CoI)_{sun}_phys.abundfloatCoILine-to-line scatter (standard deviation) of A(CoI) over the number of lines used (1)phys.atmol.numberfloato_NiINumber of individual spectral lines used to derive the abundance of NiImeta.numberintA(NiI)Mean abundance log(N(NiI)/N(H))+12phys.abundfloat[NiI/H]Abundance relative to the Sun, A(NiI)-A(NiI)_{sun}_phys.abundfloats_NiILine-to-line scatter (standard deviation) of A(NiI) over the number of lines used (1)phys.atmol.numberfloato_CuI? Number of individual spectral lines used to derive the abundance of CuImeta.numberintnullableA(CuI)? Mean abundance log(N(CuI)/N(H))+12phys.abundfloatnullable[CuI/H]? Abundance relative to the Sun, A(CuI)-A(CuI)_{sun}_phys.abundfloatnullables_CuI? Line-to-line scatter (standard deviation) of A(CuI) over the number of lines used (1)phys.atmol.numberfloatnullableo_ZnINumber of individual spectral lines used to derive the abundance of ZnImeta.numberintA(ZnI)Mean abundance log(N(ZnI)/N(H))+12phys.abundfloat[ZnI/H]Abundance relative to the Sun, A(ZnI)-A(ZnI)_{sun}_phys.abundfloats_ZnI? Line-to-line scatter (standard deviation) of A(ZnI) over the number of lines used (1)phys.atmol.numberintnullableo_YIINumber of individual spectral lines used to derive the abundance of YIImeta.numberintA(YII)Mean abundance log(N(YII)/N(H))+12phys.abundfloat[YII/H]Abundance relative to the Sun, A(YII)-A(YII)_{sun}_phys.abundfloats_YIILine-to-line scatter (standard deviation) of A(YII) over the number of lines used (1)phys.atmol.numberfloato_ZrIINumber of individual spectral lines used to derive the abundance of ZrIImeta.numberintA(ZrII)Mean abundance log(N(ZrII)/N(H))+12phys.abundfloat[ZrII/H]Abundance relative to the Sun, A(ZrII)-A(ZrII)_{sun}_phys.abundfloats_ZrII? Line-to-line scatter (standard deviation) of A(ZrII) over the number of lines used (1)phys.atmol.numberfloatnullableo_MoI? Number of individual spectral lines used to derive the abundance of MoImeta.numberintnullableA(MoI)? Mean abundance log(N(MoI)/N(H))+12phys.abundfloatnullable[MoI/H]? Abundance relative to the Sun, A(MoI)-A(MoI)_{sun}_phys.abundfloatnullables_MoI? Line-to-line scatter (standard deviation) of A(MoI) over the number of lines used (1)phys.atmol.numberfloatnullableo_BaIINumber of individual spectral lines used to derive the abundance of BaIImeta.numberintA(BaII)Mean abundance log(N(BaII)/N(H))+12phys.abundfloat[BaII/H]Abundance relative to the Sun, A(BaII)-A(BaII)_{sun}_phys.abundfloats_BaII? Line-to-line scatter (standard deviation) of A(BaII) over the number of lines used (1)phys.atmol.numberfloatnullableo_LaIINumber of individual spectral lines used to derive the abundance of LaIImeta.numberintA(LaII)Mean abundance log(N(LaII)/N(H))+12phys.abundfloat[LaII/H]Abundance relative to the Sun, A(LaII)-A(LaII)_{sun}_phys.abundfloats_LaIILine-to-line scatter (standard deviation) of A(LaII) over the number of lines used (1)phys.atmol.numberfloato_CeIINumber of individual spectral lines used to derive the abundance of CeIImeta.numberintA(CeII)Mean abundance log(N(CeII)/N(H))+12phys.abundfloat[CeII/H]Abundance relative to the Sun, A(CeII)-A(CeII)_{sun}_phys.abundfloats_CeII? Line-to-line scatter (standard deviation) of A(CeII) over the number of lines used (1)phys.atmol.numberfloatnullableo_PrII? Number of individual spectral lines used to derive the abundance of PrIImeta.numberintnullableA(PrII)? Mean abundance log(N(PrII)/N(H))+12phys.abundfloatnullable[PrII/H]? Abundance relative to the Sun, A(PrII)-A(PrII)_{sun}_phys.abundfloatnullables_PrII? Line-to-line scatter (standard deviation) of A(PrII) over the number of lines used (1)phys.atmol.numberfloatnullableo_NdIINumber of individual spectral lines used to derive the abundance of NdIImeta.numberintA(NdII)Mean abundance log(N(NdII)/N(H))+12phys.abundfloat[NdII/H]Abundance relative to the Sun, A(NdII)-A(NdII)_{sun}_phys.abundfloats_NdIILine-to-line scatter (standard deviation) of A(NdII) over the number of lines used (1)phys.atmol.numberfloato_SmIINumber of individual spectral lines used to derive the abundance of SmIImeta.numberintA(SmII)Mean abundance log(N(SmII)/N(H))+12phys.abundfloat[SmII/H]Abundance relative to the Sun, A(SmII)-A(SmII)_{sun}_phys.abundfloats_SmII? Line-to-line scatter (standard deviation) of A(SmII) over the number of lines used (1)phys.atmol.numberfloatnullableo_EuIINumber of individual spectral lines used to derive the abundance of EuIImeta.numberintA(EuII)Mean abundance log(N(EuII)/N(H))+12phys.abundfloat[EuII/H]? Abundance relative to the Sun, A(EuII)-A(EuII)_{sun}_phys.abundfloatnullables_EuII? Line-to-line scatter (standard deviation) of A(EuII) over the number of lines used (1)phys.atmol.numberfloatnullable