J/A+A/608/A89ivo://CDS.VizieR/J/A+A/608/A89doi:10.26093/cds/vizier.36080089CDSMashonkina L.Jablonka P.Sitnova TPakhomov YuNorth P.2017-12-15T18:15:50Z2017-12-11T07:42:02ZCDS support team

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

cds-question@unistra.frgiant-starschemically-peculiar-starsspectroscopychemical-abundancesastronomical-modelsstellar-atmospheresgalaxiesWe present the non-local thermodynamic equilibrium (NLTE) abundances of up to 10 chemical species in a sample of 59 very metal-poor (VMP, -4<=[Fe/H]<~-2) stars in seven dwarf spheroidal galaxies (dSphs) and in the Milky Way (MW) halo. Our results are based on high-resolution spectroscopic datasets and homogeneous and accurate atmospheric parameters determined in Paper I. We show that once the NLTE effects are properly taken into account, all massive galaxies in our sample, that is, the MW halo and the classical dSphs Sculptor, Ursa Minor, Sextans, and Fornax, reveal a similar plateau at [alpha/Fe]=0.3 for each of the alpha-process elements: Mg, Ca, and Ti. We put on a firm ground the evidence for a decline in alpha/Fe with increasing metallicity in the Bootes I ultra-faint dwarf galaxy (UFD), that is most probably due to the ejecta of type Ia supernovae. For Na/Fe, Na/Mg, and Al/Mg, the MW halo and all dSphs reveal indistinguishable trends with metallicity, suggesting that the processes of Na and Al synthesis are identical in all systems, independent of their mass. The dichotomy in the [Sr/Ba] versus [Ba/H] diagram is observed in the classical dSphs, similarly to the MW halo, calling for two different nucleosynthesis channels for Sr. We show that Sr in the massive galaxies is better correlated with Mg than Fe and that its origin is essentially independent of Ba, for most of the [Ba/H] range. Our three UFDs, that is Bootes I, UMa II, and Leo IV, are depleted in Sr and Ba relative to Fe and Mg, with very similar ratios of [Sr/Mg]=-1.3 and [Ba/Mg]=-1 on the entire range of their Mg abundances. The subsolar Sr/Ba ratios of Bootes I and UMa II indicate a common r-process origin of their neutron-capture elements. Sculptor remains the classical dSph, in which the evidence for inhomogeneous mixing in the early evolution stage, at [Fe/H]<-2, is the strongest.2017A&A...608A..89Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/608/A89CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/604/A129 : Formation of MW halo and its dwarf satellites (Mashonkina+,J/AJ/144/168 : Spectroscopy of Scl 1019417 and UMi 20103 (Kirby+, 2012)J/ApJ/802/93 : 5 stars in Sculptor chemical abundance analysis (Simon+, 2015)J/ApJ/719/931 : Chemical evolution of the UMi dSph (Cohen+, 2010)J/ApJ/763/61 : Abundances of 7 red giant members of BootesI (Gilmore+, 2013)J/ApJ/711/350 : Metal-poor giant Boo-1137 abundances (Norris+, 2010)J/ApJ/826/110 : Boo-127 and Boo-980 high-resolution spectra (Frebel+, 2016)J/ApJ/708/560 : Spectroscopy of UMa II and Coma Ber (Frebel+, 2010)J/ApJ/778/56 : Hamburg/ESO Survey extremely metal-poor stars (Cohen+, 2013)J/A+A/516/A46 : HE 2327-5642 abundance analysis (Mashonkina+, 2010)J/A+A/569/A43 : HE 2252-4225 abundance analysis (Mashonkina+, 2014)J/A+A/604/A129 : Formation of MW halo and its dwarf satelliteshttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/608/A89https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/608/A89http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/608/A89https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/608/A89https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/608/A89http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/608/A89GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/608/A89/sources (stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/608/A89/sources?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/608/A89/sources?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/608/A89/sources?GETtext/xml+votable180.050000true15.054-33.70108330.0055555555555555566/7416-7417 8744-8745 8766 11690-11691 12032 16821 16893 17035 17081 17099 17419 17578 17938 18086 18425 25719 25991 26347 26457 26980 27207 27218 34775 35477 35549 35551 35720 35969 36135 36691 44208 44797 46155 46490https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/608/A89?format=asciiOpticaldefaultJ/A+A/608/A89/table3LTE and NLTE abundances from individual lines in the starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar designationmeta.id;meta.maincharElAtomphys.atmol.elementcharIonIonphys.atmol.ionStagecharlambdaWavelength0.1nmem.wlfloatEexcExcitation energyeVphys.atmol.excitationfloatloggfAdopted gf-valuephys.absorption.coefffloatG6/NHvan der Waals damping constant log(G6/NH) at 10000Krad.s**-1.cm**-3phys.damping;arith.zpfloatEW? Equivalent width (-1 means using spectral synthesis)0.1pmspect.line.eqWidthfloatnullableepsLTELTE abundance (logeps(H)=12)phys.abundfloatepsNLTE? NLTE abundance (logeps(H)=12)phys.abundfloatnullableJ/A+A/608/A89/sourcesstarsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar designationmeta.id;meta.maincharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainSNameSimbad namemeta.idcharPapIDisplay the paper I data (Mashonkina et al., 2017, Cat. J/A+A/604/A129meta.ref.urlcharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/A+A/608/A89/table4Summary of the LTE and NLTE abundances of the investigated starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar designationmeta.id;meta.maincharNelAtomic numbermeta.idintElAtomphys.atmol.elementcharIonIonphys.atmol.ionStagecharNlinNumber of linesmeta.numberintepsLTE? LTE abundance (logeps(H)=12)phys.abundfloatnullablee_epsLTE? LTE abundance dispersionstat.errorfloatnullable[El/H]? LTE abundance [El/H]log(Sun)phys.abundfloatnullable[El/Fe]? LTE abundance [El/Fe]log(Sun)phys.abundfloatnullableepsNLTE? NLTE abundance (logeps(H)=12)phys.abundfloatnullablee_epsNLTE? NLTE abundance dispersionstat.errorfloatnullable[El/Fe]N? NLTE abundance [El/Fe]log(Sun)phys.abundfloatnullableMethodMethod of analysis (1)meta.notechar