J/A+A/694/A248ivo://CDS.VizieR/J/A+A/694/A248doi:10.26093/cds/vizier.36940248CDSLatour M.Kamann S.Martocchia S.Husser T.-O.Saracino S.Dreizler S.2025-05-21T20:01:51Z2025-02-18T09:20:52ZCDS support team

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

cds-question@unistra.frglobular-star-clustersspectroscopymetallicityMultiple populations are ubiquitous in the old massive globular clusters (GCs) of the Milky Way. It is still unclear how they arose during the formation of a GC. The topic of iron and metallicity variations has recently attracted attention with the measurement of iron variations among the primordial population (P1) stars of Galactic GCs. We use the spectra of more than 8000 RGB stars in 21 Galactic GCs observed with MUSE to derive individual stellar metallicities [M/H]. For each cluster, we use the HST photometric catalogs to separate the stars into two main populations (P1 and P2). We measure the metallicity spread within the primordial population of each cluster by combining our metallicity measurements with the stars {Delta}_F275W,F814W_ pseudo-color. We also derive metallicity dispersions ({sigma}_[M/H]_) for the P1 and P2 stars of each GC. In all but three GCs, we measure a significant correlation between the metallicity and the {Delta}_F275W,F814W_ pseudo-color of the P1 stars such that stars with larger {Delta_F275W,F814W_ have higher metallicities. We measure metallicity spreads that range from 0.03 to 0.24dex and correlate with the GC masses. As for the intrinsic metallicity dispersions, when combining the P1 and P2 stars, we measure values ranging from 0.02 dex to 0.08dex that correlate very well with the GC masses. We compared the metallicity dispersion among the P1 and P2 stars and found that the P2 stars have metallicity dispersions that are smaller or equal to that of the P1 stars. We find that both the metallicity spreads of the P1 stars (from the {Delta_F275W,F814W_ spread in the chromosome maps) and the metallicity dispersions ({sigma_[M/H]_) correlate with the GC masses, as predicted by some theoretical self-enrichment models presented in the literature.2025A&A...694A.248Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/694/A248CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/635/A114 : EW and [Fe/H] for 30000 globular cluster RGB starshttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/694/A248https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/694/A248http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/694/A248https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/694/A248https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/694/A248http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/694/A248GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/694/A248/table1 (Properties of the RGB stars in our spectral sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/694/A248/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/694/A248/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/694/A248/table1?GETtext/xml+votable180.050000true6.0627352-72.09532620.0055555555555555566/12405 19091 28705 28751 28972-28973 31019 31115 31417 33321 33330 34242 37294 38465 41304 42314 42990 43125 47125 47168 47777 47868 48434https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/694/A248?format=asciidefaultJ/A+A/694/A248/table1Properties of the RGB stars in our spectral samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSourceStar identification numbermeta.id;meta.mainintRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainClusterCluster namemeta.id.assocchar[M/H]Metallicitylog(Sun)phys.abund.Zfloate_[M/H]Error on the metallicitylog(Sun)stat.error;phys.abundfloatTeffEffective temperatureKphys.temperature.effectiveinte_TeffError on the effective temperatureKstat.error;phys.temperature.effectiveintSNRAverage signal-to-noise of the Nspec spectrastat.snr;stat.meanintNspecNumber of spectra used to average Teff and [M/H]meta.numberintloggSurface gravitylog(cm.s**-2)phys.gravityfloate_loggError on the surface gravity (1)log(cm.s**-2)stat.errorfloatCMxDelta(F275W,F814W), X-axis position on the Chromosome mapstat.fit.paramfloatCMyDeltaC(F275W,F336W,F438W), Y-axis position on the Chromosome mapstat.fit.paramfloatP1[0/1] =1 if the star belongs to P1meta.codeintP2[0/1] =1 if the star belongs to P2meta.codeint