J/A+A/584/A86ivo://CDS.VizieR/J/A+A/584/A86doi:10.26093/cds/vizier.35840086CDSSiqueira-Mello C.Andrievsky S.M.Barbuy B.Spite M.Spite F.,Korotin S.A.2015-11-25T07:03:46Z2015-11-25T08:03:06ZCDS support team

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

cds-question@unistra.frhalo-starspopulation-ii-starschemical-abundancesHD 140283 is a reference subgiant that is metal poor and confirmed to be a very old star. The abundances of this type of old star can constrain the nature and nucleosynthesis processes that occurred in its (even older) progenitors. The present study may shed light on nucleosynthesis processes yielding heavy elements early in the Galaxy. A detailed abundance analysis of a high-quality spectrum is carried out, with the intent of providing a reference on stellar lines and abundances of a very old, metal-poor subgiant.2015A&A...584A..86Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/584/A86CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/584/A86https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/584/A86http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/584/A86https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/584/A86https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/584/A86http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/584/A86GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/584/A86/tablea1Fe and Ti lines adopted. Atomic data and abundancesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElElement and degree of ionizationphys.atmol.element;phys.atmol.ionizationcharlambdaWavelength of the line0.1nmem.wl;spect.linedoublechiexExcitation potentialeVphys.atmol.excitationfloatloggfVALDOscillator strength of the transition from VALD databasephys.atmol.wOscStrength;phys.atmol.transitionfloatloggfNIST? Oscillator strength of the transition from NIST databasephys.atmol.wOscStrength;phys.atmol.transitionfloatnullableEWEquivalent widths0.1pmspect.line.eqWidthfloate_EWError on the equivalent widths (1)0.1pmstat.error;spect.line.eqWidthfloatA(X)Elemental abundances (G1)phys.abundfloate_A(X)Error on the elemental abundancesstat.errorfloatJ/A+A/584/A86/tablea2Line by line elemental abundancesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSpeciesElement and degree of ionizationphys.atmol.element;phys.atmol.ionizationcharlambdaWavelength of the line0.1nmem.wl;spect.linedoublechiexExcitation potentialeVphys.atmol.excitationfloatloggfOscillator strength of the transitionphys.atmol.wOscStrength;phys.atmol.transitionfloatl_A(X)Limit flag on A(X)meta.code.errorcharA(X)Elemental abundances (G1)phys.abundfloatl_[X/H]Limit flag on [X/H]meta.code.error;phys.abundchar[X/H]Abundance ratio (2)phys.abund;arith.ratiofloatl_[X/Fe]Limit flag on [X/Fe]meta.code.error;phys.abundchar[X/Fe]Abundance ratiophys.abundfloatJ/A+A/584/A86/tablea3Hyperfine coupling constantsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElIsotope and degree of ionizationphyscharlambdaWavelength of the line0.1nmem.wl;spect.linedoubleJLowerTotal angular momentum of the lower levelmeta.idfloatALower? HFS A coefficient of the lower levelMHzphys.atmoldoublenullableBLower? HFS B coefficient of the lower levelMHzphys.atmolfloatnullabler_JLower? Reference for the HFS coefficients of the lower level (1)meta.ref;pos.frameintnullableJUpperTotal angular momentum of the upper levelmeta.idfloatAUpper? HFS A coefficient of the upper levelMHzphys.atmoldoublenullableBUpper? HFS B coefficient of the upper levelMHzphys.atmolfloatnullabler_JUpper? Reference for the HFS coefficients of the upper level (1)meta.ref;pos.frameintnullable