J/A+A/594/A79ivo://CDS.VizieR/J/A+A/594/A79doi:10.26093/cds/vizier.35940079CDSSpite M.Spite F.Gallagher A.J.Monaco L.Bonifacio P.Caffau E.,Villanova S.2018-03-13T16:05:23Z2016-10-14T09:06:08ZCDS support team

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

cds-question@unistra.frglobular-star-clusterspopulation-ii-starschemical-abundancesThe stellar abundances observed in globular clusters show complex structures, currently not yet understood. The aim of this work is to investigate the relations between the abundances of different elements in the globular cluster M4, selected for its uniform deficiency of iron, to explore the best models explaining the pattern of these observed abundances. Moreover, in turnoff stars, the abundances of the elements are not suspected to be affected by internal mixing. In M4, using low and moderate resolution spectra obtained for 91 turnoff (and subgiant) stars with the ESO FLAMESGiraffe spectrograph, we have extended previous measurements of abundances (of Li, C and Na) to other elements (C, Si, Ca, Sr and Ba), using model atmosphere analysis. We have also studied the influence of the choice of the microturbulent velocity. Firstly, the peculiar turnoff star found to be very Li-rich in a previous paper does not show any other abundance anomalies relative to the other turnoff stars inM4. Secondly, an anti-correlation between C and Na has been detected, the slope being significative at more than 3{sigma}. This relation between C and Na is in perfect agreement with the relation found in giant stars selected below the RGB bump. Thirdly, the strong enrichment of Si and of the neutron-capture elements Sr and Ba, already observed in the giants in M4, is confirmed. Finally, the relations between Li, C, Na, Sr and Ba constrain the enrichment processes of the observed stars. The abundances of the elements in the turnoff stars appear to be compatible with production processes by massive AGBs, but are also compatible with the production of second generation elements (like Na) and low Li produced by, for example, fast rotating massive stars.2016A&A...594A..79Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/594/A79CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/539/A157 : Li and Na in globular cluster M4 (Monaco+, 2012)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/594/A79https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/594/A79http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/594/A79https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/594/A79https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/594/A79http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/594/A79GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/594/A79/table3Abundances measured in our M4 stars computed with the model parameters Teff logg and vt given by Monaco et al. (2012, Cat. J/A+A/539/A157)Nacorr? [Na/Fe]nonLTE - [Na/Fe]LTEarith.factorfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintM12Display the data of Monaco et al. (2012, Cat, J/A+A/539/A157)meta.ref.urlcharIDStar identification, [MVB2012] NNNNN in Simbadmeta.id;meta.mainint[Fe/H]Metallicity (from qdopted model)log(Sun)phys.abund.Zfloat[Na/Fe]? non-LTE relative abundance [Na/Fe]log(Sun)phys.abundfloatnullableA(Li)? Logarithmic abundance of Liphys.abundfloatnullable[C/Fe]? Relative abundance [C/Fe] (3D computations)log(Sun)phys.abundfloatnullable[Si/Fe]? Relative abundance [Si/Fe]log(Sun)phys.abundfloatnullable[Ca/Fe]? Relative abundance [Ca/Fe]log(Sun)phys.abundfloatnullable[Ni/Fe]? Relative abundance [Ni/Fe]log(Sun)phys.abundfloatnullable[Sr/Fe]? Relative abundance [Sr/Fe]log(Sun)phys.abundfloatnullable[Ba/Fe]? Relative abundance [Ba/Fe]log(Sun)phys.abundfloatnullablef_[Ba/Fe][*] * when [Ba/Fe] from only the 4554{AA} linemeta.codecharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/A+A/594/A79/table4Abundances measured in our M4 stars computed with the model parameters Teff logg given by Monaco et al. (2012, Cat. J/A+A/539/A157) but with vt=1.3km/srecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintM12Display the data of Monaco et al. (2012, Cat, J/A+A/539/A157)meta.ref.urlcharIDStar identification, [MVB2012] NNNNN in Simbadmeta.id;meta.mainint[Fe/H]Metallicity (from qdopted model)log(Sun)phys.abund.Zfloat[Na/Fe]? non-LTE relative abundance [Na/Fe]log(Sun)phys.abundfloatnullableNacorr? [Na/Fe]nonLTE - [Na/Fe]LTEarith.factorfloatnullableA(Li)? Logarithmic abundance of Liphys.abundfloatnullable[C/Fe]? Relative abundance [C/Fe] (3D computations)log(Sun)phys.abundfloatnullable[Si/Fe]? Relative abundance [Si/Fe]log(Sun)phys.abundfloatnullable[Ca/Fe]? Relative abundance [Ca/Fe]log(Sun)phys.abundfloatnullable[Ni/Fe]? Relative abundance [Ni/Fe]log(Sun)phys.abundfloatnullable[Sr/Fe]? Relative abundance [Sr/Fe]log(Sun)phys.abundfloatnullable[Ba/Fe]? Relative abundance [Ba/Fe]log(Sun)phys.abundfloatnullablef_[Ba/Fe][*] * when [Ba/Fe] from only the 4554{AA} linemeta.codecharSimbadSimbad column added by the CDSmeta.ref.urlchar