J/A+A/620/A187ivo://CDS.VizieR/J/A+A/620/A187doi:10.26093/cds/vizier.36200187CDSFrancois P.Caffau E.Bonifacio P.Spite M.Spite F.Cayrel R.,Christlieb N.Gallagher A.Klessen R.Koch A.Ludwig H.-G.Monaco L.,Plez B.Steffen M.Zaggia S.2020-06-19T12:34:59Z2018-12-14T09:41:07ZCDS support team

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

cds-question@unistra.frchemically-peculiar-starschemical-abundancesmilky-way-galaxyExtremely metal-poor stars are keys to understand the early evolution of our Galaxy. The ESO large programme TOPoS has been tailored to analyse a new set of metal-poor turn-off stars, whereas most of the previously known extremely metal-poor stars are giant stars. Our results confirms the super-solar [Mg/Fe] and [Ca/Fe] ratios in metal-poor turn-off stars as observed in metal-poor giant stars. We found a significant spread of the [alpha/Fe] ratios with several stars showing sub-solar [Ca/Fe] ratios. We could measure the abundance of strontium in 12 stars of the sample, leading to abundance ratios [Sr/Fe] around the Solar value. We detected barium in two stars of the sample. One of the stars (SDSS J114424-004658) shows both very high [Ba/Fe] and [Sr/Fe] abundance ratios (>1dex).2018A&A...620A.187Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/620/A187CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/579/A28 : Abundances of 3 CEMP stars (Bonifacio+, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/620/A187https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/620/A187http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/620/A187https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/620/A187https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/620/A187http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/620/A187GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/620/A187/tablea1 (Stellar Parameters)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/620/A187/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/620/A187/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/620/A187/tablea1?GETtext/xml+votable180.050000true1.048375-5.84105560.0055555555555555566/27 2067 4296 4542 4713 4751 5141 6216 8547 8666 8670 8699 8857 10251 10275 17240 17357 17555 17645 17849 17858 17907 18004 18067-18068 18391 18521 18881 18891 19007 19030 19047 19143 19267 19328 19366 19686 21996 22715 23060 23213 25332-25333 25530 25985 26050 26114 26161 26169 26203 26205 26265 26495 26549 26968 27023 27041 27446 27846 27939 29777 31403 32651 32672 409511.9867573869263685e-19 3.916500758235022e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/620/A187?format=asciidefaultJ/A+A/620/A187/tablea1Stellar ParametersSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSDSSSDSS star identification (JHHMMSS+DDMMSS)meta.id;meta.maincharTeffEffective temperatureKphys.temperature.effectiveint[Fe/H]Metallicityphys.abund.ZfloatRAJ2000Right ascension (J2000.0)pos.eq.ra;meta.mainDEJ2000Declination (J2000.0)pos.eq.dec;meta.mainGmagGaia G magnitudemagphot.mag;em.optfloatSNRSignal to Noise ratiostat.snrintNameSDSS DR12 name (SDSS JHHMMSS.ss+DDMMSS.s)meta.idcharSloanDisplay the online SDSS data for this objectmeta.ref.urlcharJ/A+A/620/A187/tablea2Chemical composition of the stars analysed in this papernSr? Number of lines used to determine the abundance of Srmeta.numberintnullable[Ba/Fe]? Abundance [Ba/Fe]phys.abundfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSDSSSDSS star identification (JHHMMSS+DDMMSS)meta.id;meta.mainchar[Fe/H]Metallicityphys.abund.Zfloatl_A(C)Upper limit flag on A(C)meta.code.errorcharA(C)Carbon abundance (upper limit)phys.abundfloat[Mg/Fe]? Abundance [Mg/Fe]phys.abundfloatnullablenMg? Number of lines used to determine the abundance of Mgmeta.numberintnullable[Ca/Fe]? Abundance [Ca/Fe]phys.abundfloatnullablenCa? Number of lines used to determine the abundance of Cameta.numberintnullable[Si/Fe]? Abundance [Si/Fe]phys.abundfloatnullablenSi? Number of lines used to determine the abundance of Simeta.numberintnullable[Sr/Fe]? Abundance [Sr/Fe]phys.abundfloatnullablenBa? Number of lines used to determine the abundance of Bameta.numberintnullableJ/A+A/620/A187/tablea3Equivalent width of Fe lines used to determine the metallicity of the starsElElementphys.atmol.elementcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSDSSSDSS star identification (JHHMMSS+DDMMSS)meta.id;meta.maincharLambdaWavelengthnmem.wldoubleEWEquivalent width (m{AA})0.1pmspect.line.eqWidthint