J/A+A/585/A150ivo://CDS.VizieR/J/A+A/585/A150doi:10.26093/cds/vizier.35850150CDSNetopil M.Paunzen E.Heiter U.Soubiran C.2018-01-08T06:38:05Z2016-05-10T13:46:19ZCDS support team

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

cds-question@unistra.fropen-star-clustersmetallicityOpen clusters are known as excellent tools for various topics in Galactic research. For example, they allow accurately tracing the chemical structure of the Galactic disc. However, the metallicity is known only for a rather low percentage of the open cluster population, and these values are based on a variety of methods and data. Therefore, a large and homogeneous sample is highly desirable. In the third part of our series we compile a large sample of homogenised open cluster metallicities using a wide variety of different sources. These data and a sample of Cepheids are used to investigate the radial metallicity gradient, age effects, and to test current models. We used photometric and spectroscopic data to derive cluster metallicities. The different sources were checked and tested for possible offsets and correlations. In total, metallicities for 172 open cluster were derived. We used the spectroscopic data of 100 objects for a study of the radial metallicity distribution and the age-metallicity relation. We found a possible increase of metallicity with age, which, if confirmed, would provide observational evidence for radial migration. Although a statistical significance is given, more studies are certainly needed to exclude selection effects, for example. The comparison of open clusters and Cepheids with recent Galactic models agrees well in general. However, the models do not reproduce the flat gradient of the open clusters in the outer disc. Thus, the effect of radial migration is either underestimated in the models, or an additional mechanism is at work. Apart from the Cepheids, open clusters are the best tracers for metallicity over large Galactocentric distances in the Milky Way. For a sound statistical analysis, a sufficiently large and homogeneous sample of cluster metallicities is needed. Our compilation is currently by far the largest and provides the basis for several basic studies such as the statistical treatment of the Galactic cluster population, or evolutionary studies of individual star groups in open clusters.2016A&A...585A.150Nhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/585/A150CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/561/A93 : On the metallicity of open clusters. II. (Heiter+, 2014)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/585/A150https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/585/A150http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/585/A150https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/585/A150https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/585/A150http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/585/A150GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/585/A150/tablea1 (Metallicities of the open clusters)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/585/A150/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/585/A150/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/585/A150/tablea1?GETtext/xml+votable180.050000true50.425-36.30.0055555555555555566/463 1302 1385 1481 1514 1582 1653 1923 2395 2436 3015 3063 3076 3091 3136 3168 3604 3633 3640 4078 4298 4698 6149 12990 13198 13996 14033 14059 14175 14210 14221 14246 14324 14336 14575 14740 14752 15121 15595 15711 15759 15827 16490 20562 20763 20797 20814 20903 20939 20957 20989 21372 21523 21529 21531 21538 21557 21586 21647 21719 21774 22058 22111 22123 22130 22216 22235 22239 22433 22499 22805 22871 22887 23410 23538 23612 23633 23637-23638 23745 23761 23861 23964 24057 24121 24330 24344-24345 24491 24522 24544 28481 28711 28806 28818 28822 28825 29066 29081 29106 29269 29728 30215 30308 30439 30506 31790 31812 33099 34495 37231 37237 37351 37592 37705 37790 37867 37920 37933 37971 38073 38242 38432 39131 39181 39213 39251 39274 39354 39356 39374 39697 39739 39770 39775 39883 39901 39912 40071 40104 40490 40696 41461 41613 41649 41670 41682 41688 41696 41699 41710 41809 41834 41863 42135 42153 42155 42159 42177 42203 42216 42274 42399 42402 42464 43022 43034 43044 43140 43301https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/585/A150?format=asciidefaultJ/A+A/585/A150/tablea1Metallicities of the open clustersSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClusterCluster namemeta.id;meta.mainchar[Fe/H]HQS? Metallicity from high-quality spectroscopic data data (HQS)phys.abund.Fefloatnullablee_[Fe/H]HQS? rms uncertainty on [Fe/H]HQSstat.error;phys.abund.FefloatnullableN[Fe/H]HQS? Number of stars used for the calculation of [Fe/H]HQSmeta.numberintnullable[Fe/H]LQS? Metallicity from low-quality spectroscopic data data (LQS)phys.abund.Fefloatnullablee_[Fe/H]LQS? rms uncertainty on [Fe/H]LQSstat.error;phys.abund.FefloatnullableN[Fe/H]LQS? Number of stars used for the calculation of [Fe/H]LQSmeta.numberintnullable[Fe/H]Phot? Metallicity from photometryphys.abund.Fefloatnullablee_[Fe/H]Phot? rms uncertainty on [Fe/H]Photstat.error;phys.abund.Fefloatnullablew_[Fe/H]Phot? Total weight of the photometric metallicitiesstat.weightfloatnullableSystemsCode for the photometric systems (1)meta.codecharRGCMean distance from the Sunkpcpos.distance;pos.heliocentricfloate_RGCrms uncertainty on RGCkpcstat.errorfloatAgeAgeGyrtime.agefloate_Agerms uncertainty on AgeGyrstat.error;time.agefloatNNumber of studies used to calculate the mean distance from the Sun and the age of the open clustermeta.numberint_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.main