J/A+A/579/A104ivo://CDS.VizieR/J/A+A/579/A104doi:10.26093/cds/vizier.35790104CDSSbordone L.Monaco L.Moni Bidin C.Bonifacio P.Villanova S.,Bellazzini M.Ibata R.Chiba M.Geisler D.Caffau E.Duffau S.2018-01-31T06:09:53Z2015-07-08T09:26:19ZCDS support team

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

cds-question@unistra.frglobular-star-clustersgiant-starsline-intensitiesspectroscopymetallicityThe tidal disruption of the Sagittarius dwarf Spheroidal galaxy (Sgr dSph) is producing the most prominent substructure in the Milky Way (MW) halo, the Sagittarius Stream. Aside from field stars, the Sgr dSph is suspected to have lost a number of globular clusters (GC). Many Galactic GC are suspected to have originated in the Sgr dSph. While for some candidates an origin in the Sgr dSph has been confirmed due to chemical similarities, others exist whose chemical composition has never been investigated. NGC 5053 and NGC 5634 are two among these scarcely studied Sgr dSph candidate-member clusters. To characterize their composition we analyzed one giant star in NGC 5053, and two in NGC 5634. We analize high-resolution and signal-to-noise spectra by means of the MyGIsFOS code, determining atmospheric parameters and abundances for up to 21 species between O and Eu. The abundances are compared with those of MW halo field stars, of "unassociated" MW halo globulars, and of the metal poor Sgr dSph main body population. We derive a metallicity of [FeII/H]=-2.26+/-0.10 for NGC 5053, and of [FeI/H]=-1.99+/-0.075 and -1.97+/-0.076 for the two stars in NGC 5634. This makes NGC 5053 one of the most metal poor globular clusters in the MW. Both clusters display an alpha enhancement similar to the one of the halo at comparable metallicity. The two stars in NGC 5634 clearly display the Na-O anticorrelation widespread among MW globulars. Most other abundances are in good agreement with standard MW halo trends. The chemistry of the Sgr dSph main body populations is similar to the one of the halo at low metallicity. It is thus difficult to discriminate between an origin of NGC 5053 and NGC 5634 in the Sgr dSph, and one in the MW. However, the abundances of these clusters do appear closer to that of Sgr dSph than of the halo, favoring an origin in the Sgr dSph system.2015A&A...579A.104Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/579/A104CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/579/A104https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/579/A104http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/579/A104https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/579/A104https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/579/A104http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/579/A104GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/579/A104/table1 (*Coordinates, photometry, heliocentric radial velocities, and determined atmospheric parameters for the three targets)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/579/A104/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/579/A104/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/579/A104/table1?GETtext/xml+votable180.050000true199.149833317.68688890.0055555555555555566/25873 27984https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/579/A104?format=asciiOpticaldefaultJ/A+A/579/A104/alllinesPer-feature fit resultso_FeatDetails of featuremeta.numberintnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar namemeta.id;meta.maincharElElement namemeta.id;phys.atmol.elementcharZ[8/63] Atomic numbermeta.idintIon[0/1] Ionization state (1)phys.atmol.ionStageintWini[481/671] Starting wavelength of fitted featurenmspect.line.eqWidth;meta.modelleddoubleWend[481/671] Ending wavelength of fitted featurenmspect.line.eqWidth;meta.modelleddouble[X/H][-3/-1] Abundance of the element in [X/H] formatlog(Sun)phys.abundfloatEWf[2/19] Equivalent width of the best fitting synthetic featurepmspect.line.eqWidth;meta.modelledfloatEWo[2/19] Equivalent width of the observed featurepmspect.line.eqWidthfloatS/N[46-94] Signal-to-noise ratio at feature centerstat.snrfloatShift[-4/2] Doppler shift applied to the featurekm/sspect.dopplerVelocfloatCont[0.99/1.01] Feature continuum renormalizationphot.flux.density;arith.ratiofloatVTuse[0/1] Flag for use in Vt determination (2)meta.codeintTuse[0/1] Flag for use in Teff determination (3)meta.codeintFeatFeature ID (4)meta.id;spect.linecharprimaryJ/A+A/579/A104/allsynthFeature observed and best-fitting profilesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar namemeta.id;meta.maincharFeatFeature IDmeta.id;spect.linecharlambda[481/671] Wavelength {lambda}nmem.wldoubleFsynth[0.2/1.1] Best-fitting synthetic normalized flux (1)phot.flux;arith.ratiofloatFobs[0.2/1.1] Observed normalized fluxphot.flux;arith.ratiofloatJ/A+A/579/A104/table1*Coordinates, photometry, heliocentric radial velocities, and determined atmospheric parameters for the three targetsTeff[4085/4450] Effective temperatureKphys.temperature.effectiveintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNGCCluster NGC numbermeta.id.parentintStarStar namemeta.id;meta.maincharprimaryNfNumber of features observed for this starmeta.numberintnullableRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainVmag[14.5/14.8] V magnitudemagphot.mag;em.opt.VfloatV-IV-I colour indexmagphot.color;em.opt.V;em.opt.IfloatHRV[-21/43] Heliocentric radial velocitykm/sspect.dopplerVeloc;pos.heliocentricfloatlogg[0.2/1.2] Surface gravitylog(cm.s**-2)phys.gravityfloatVturbMicroturbulent velocitykm/sphys.velocfloat[Fe/H][-2.3/-1.9] Metallicitylog(Sun)phys.abund.Zfloatn_[Fe/H][a] a: using [FeII/H] for this starmeta.notechar