J/A+A/590/A9ivo://CDS.VizieR/J/A+A/590/A9doi:10.26093/cds/vizier.35900009CDSDias B.Barbuy B.Saviane IHeld E.Da Costa G.Ortolani S.,Gullieuszik M.Vasquez S.2016-04-28T07:46:20Z2016-04-28T08:41:07ZCDS support team

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

cds-question@unistra.frmilky-way-galaxyglobular-star-clustersgiant-starschemical-abundancesradial-velocityspectroscopyeffective-temperatureastronomical-modelsstellar-atmospheresGlobular clusters trace the formation and evolution of the Milky Way and surrounding galaxies, and outline their chemical enrichment history. To accomplish these tasks it is important to have large samples of clusters with homogeneous data and analysis to derive kinematics, chemical abundances, ages and locations. We aim to obtain homogeneous metallicities and alpha-element enhancement for 51 Galactic bulge, disc, and halo globular clusters that are among the most distant and/or highly reddened in the Galaxy's globular cluster system. We also provide membership selection based on stellar radial velocities and atmospheric parameters. The implications of our results are discussed. We observed R~2000 spectra in the wavelength interval 456-586nm for over 800 red giant stars in 51 Galactic globular clusters. We applied full spectrum fitting with the code ETOILE together with libraries of observed and synthetic spectra. We compared the mean abundances of all clusters with previous work and with field stars. We used the relation between mean metallicity and horizontal branch morphology defined by all clusters to select outliers for discussion. [Fe/H], [Mg/Fe], and [alpha/Fe] were derived in a consistent way for almost one-third of all Galactic globular clusters. We find our metallicities are comparable to those derived from high-resolution data to within sigma=0.08dex over the interval -2.5<[Fe/H]<0.0. Further, a comparison of previous metallicity scales with ours yields sigma<0.16dex. We also find that the distribution of [Mg/Fe] and [alpha/Fe] with [Fe/H] for the 51 clusters follows the general trend exhibited by field stars. It is the first time that the following clusters are included in a large sample of homogeneous stellar spectroscopic observations and metallicity derivation: BH 176, Djorg 2, Pal 10, NGC 6426, Lynga 7, and Terzan 8. In particular, the first three clusters only had photometric metallicities previously and the available metallicity for NGC 6426 was based only on integrated spectroscopy and photometry. Two other clusters, HP 1 and NGC 6558, are confirmed as candidates for the oldest globular clusters in the Milky Way. Stellar spectroscopy in the visible at R~2000 for a large sample of globular clusters is a robust and efficient way to trace the chemical evolution of the host galaxy and to detect interesting objects for follow-up at higher-resolution and with forthcoming giant telescopes. The technique used here can also be applied to globular cluster systems in nearby galaxies with current instruments and to distant galaxies with the advent of ELTs.2016A&A...590A...9Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/590/A9CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/540/A27 : Spectroscopy in Galactic globular clusters (Saviane+, 2012)J/A+A/573/A13 : Metal abundances in 6 globular cluster (Dias+, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/590/A9https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/590/A9http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/590/A9https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/590/A9https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/590/A9http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/590/A9GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/590/A9/sample (Identification of cluster stars including photometric and kinematics information (table 1) and atmospheric parameters for RGB stars (table A2))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/590/A9/sample?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/590/A9/sample?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/590/A9/sample?GETtext/xml+votable180.050000true6.396667-72.039750.0055555555555555566/12405 12531 12943 24843 25873 28705 28717 28768-28769 28778 28838 28855 28867 28882 28972-28973 29187 29202 29219 29222 29248 29267 29294 29636-29637 29805 29816 30323 30329 30769 30995 30998 31019 31095 31417 31722-31723 31778 32083 33321 37294 38465 39642 41507 41513 41847 41852 42076 42152 42278 42528 42530 42955 43193 44086 44220 44427 47125 47168 47903 486983.322582951404819e-19 3.852589004194616e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/590/A9?format=asciiOpticaldefaultJ/A+A/590/A9/sampleIdentification of cluster stars including photometric and kinematics information (table 1) and atmospheric parameters for RGB stars (table A2)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar identification (G1)meta.id;meta.maincharCl.IDCluster identificationmeta.id.parentcharCl.NameCluster namemeta.id.parentcharRAJ2000Right ascension (J2000.0)pos.eq.ra;meta.mainDEJ2000Declination (J2000.0)pos.eq.dec;meta.mainVmagV magnitude (2)magphot.mag;em.opt.VfloatV-I? V-I colour index (2)magphot.color;em.opt.V;em.opt.IfloatnullableB-V? B-V colour index (2)magphot.color;em.opt.B;em.opt.VfloatnullableHVHeliocentric velocitykm/sspect.dopplerVeloc;pos.heliocentricintHVt? Heliocentric velocity from CaT (3)km/sphys.veloc;pos.heliocentricdoublenullableMmb[M] Membership (M=member)meta.code.membercharTeffMEffective temperature from MILES libraryKphys.temperature.effectiveinte_TeffMrms uncertainty on TeffMKstat.errorintTeffCEffective temperature from Coelho libraryKphys.temperature.effectiveinte_TeffCrms uncertainty on TeffMKstat.errorintTeffAverage of MILES and Coelho effective temperature (adopted)Kphys.temperature.effective;stat.meaninte_Teffrms uncertainty on TeffKstat.error;phys.temperature.effectiveintloggMSurface gravity from MILES librarylog(cm.s**-2)phys.gravityfloate_loggMrms uncertainty on loggMlog(cm.s**-2)stat.errorfloatloggCSurface gravity from Coelho librarylog(cm.s**-2)phys.gravityfloate_loggCrms uncertainty on loggClog(cm.s**-2)stat.errorfloatloggAverage of MILES and Coelho surface gravitylog(cm.s**-2)phys.gravity;stat.meanfloate_loggrms uncertainty on loggClog(cm.s**-2)stat.errorfloat[Fe/H]MMetallicity from MILES librarylog(Sun)phys.abund.Fefloate_[Fe/H]Mrms uncertainty on [Fe/H]Mlog(Sun)stat.error;phys.abund.Fefloat[Fe/H]CMetallicity from Coelho librarylog(Sun)phys.abund.Fefloate_[Fe/H]Crms uncertainty on [Fe/H]Clog(Sun)stat.error;phys.abund.Fefloat[Fe/H]Average of MILES and Coelho metallicitylog(Sun)phys.abund.Fefloate_[Fe/H]rms uncertainty on [Fe/H]log(Sun)stat.error;phys.abund.Fefloat[Mg/Fe]Abundance [Mg/Fe] rom MILES librarylog(Sun)phys.abundfloate_[Mg/Fe]rms uncertainty on [Mg/Fe]log(Sun)stat.error;phys.abundfloat[a/Fe]Abundance [alpha/Fe] from Coelho librarylog(Sun)phys.abundfloate_[a/Fe]rms uncertainty on [alpha/Fe]log(Sun)stat.error;phys.abundfloat