J/A+A/566/A37ivo://CDS.VizieR/J/A+A/566/A37doi:10.26093/cds/vizier.35660037CDSGenovali K.Lemasle B.Bono G.Romaniello M.Fabrizio M.Ferraro I.,Iannicola G.Laney C.D.Nonino M.Bergemann M.Buonanno R.,Francois P.Inno L.Kudritzki R.-P.Matsunaga N.Pedicelli S.,Primas F.Thevenin F.2018-01-05T08:56:57Z2014-09-24T10:41:26ZCDS support team

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

cds-question@unistra.fropen-star-clustersvariable-starschemical-abundancesWe present homogeneous and accurate iron abundances for 42 Galactic Cepheids based on high resolution (R~38000) high signal-to-noise ratio (S/N>=100) optical spectra collected with UVES at VLT (128 spectra). The above abundances were complemented with high-quality iron abundances provided either by our group (86) or available in the literature. We were careful to derive a common metallicity scale and ended up with a sample of 450 Cepheids. We also estimated accurate individual distances for the entire sample by using homogeneous near-infrared photometry and the reddening free period-Wesenheit relations. The new metallicity gradient is linear over a broad range of Galactocentric distances (R_G_~5-19kpc) and agrees quite well with similar estimates available in the literature (-0.060+/-0.002dex/kpc). We also uncover evidence that suggests that the residuals of the metallicity gradient are tightly correlated with candidate Cepheid groups (CGs). The candidate CGs have been identified as spatial overdensities of Cepheids located across the thin disk. They account for a significant fraction of the residual fluctuations, and also for the large intrinsic dispersion of the metallicity gradient. We performed a detailed comparison with metallicity gradients based on different tracers: OB stars and open clusters. We found very similar metallicity gradients for ages younger than 3Gyr, while for older ages we found a shallower slope and an increase in the intrinsic spread. The above findings rely on homogeneous age, metallicity, and distance scales. Finally, by using a large sample of Galactic and Magellanic Cepheids for which accurate iron abundances are available, we found that the dependence of the luminosity amplitude on metallicity is vanishing.2014A&A...566A..37Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/566/A37CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/511/A56 : Abundances of five open clusters (Pancino+, 2010)J/AJ/142/51 : Galactic Cepheids abundance variations (Luck+, 2011)J/AJ/142/136 : Spectroscopy of Cepheids. l=30-250{deg} (Luck+, 2011)J/A+A/554/A132 : Iron line list (FeI and FeII) (Genovali+, 2013)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/566/A37https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/566/A37http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/566/A37https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/566/A37https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/566/A37http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/566/A37GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/566/A37/table3 (Mean NIR magnitudes, mean distances and mean iron abundances for the current sample of classical Cepheids)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/566/A37/table3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/566/A37/table3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/566/A37/table3?GETtext/xml+votable180.050000true251.3296361-51.34260940.005555555555555556Cone search capability for table J/A+A/566/A37/table4 (Galactic Cepheids for which the iron abundance was available in the literature)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/566/A37/table4?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/566/A37/table4?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/566/A37/table4?GETtext/xml+votable180.050000true143.4619119-36.61576280.005555555555555556Cone search capability for table J/A+A/566/A37/table5 (Individual ages, distances, and metallicities for the current sample of open clusters)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/566/A37/table5?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/566/A37/table5?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/566/A37/table5?GETtext/xml+votable180.050000true80.1530.60.0055555555555555565/9482 6/1239 1331 1340 1348 1388 1402 1411 1421 1426 1429 1431-1432 1441 1445 1467 1481 1486 1625 1631 1765 1824 1829 1836 1858 1920 1935 1985 2436 2805 3000 3005 3008 3022 3033 3045 3047 3050 3052 3054 3059-3060 3063 3076 3091 3157 3182 3239 3252 3255 3261 3263 3277 3284-3285 3304 3306 3309 3322 3328 3336-3337 3342 3361-3362 3365 3459 3589 3599-3601 3616 3627 3629 3631-3633 3641 3645 3656 3663 3682 3712-3714 3722 3728 3731 3849 4078 4298 4698 6149 12436 12846 12934 12963 12968 12970-12971 13166 13201 13288 13309-13310 13931 13933 13961 13990 14009 14047 14059 14075 14175 14199 14205 14212 14229 14238-14239 14246 14251 14260 14262 14267 14271 14282-14283 14291-14292 14295 14301 14303 14314 14317 14320-14321 14323-14324 14328-14329 14404 14407 14409 14411 14424 14427 14430 14436 14445 14449 14453 14455 14457 14469 14533 14575 14601-14602 14607 14625 14629-14630 14634 14637 14640 14653 14690 14698 14709 14718 14736 14752 14770 15360 15378 15388 15392-15393 15396 15425 15429 15461 15585 15595 15618 15632-15633 15639 15660 15698 15759 16490 20562 20763 20814 20833 20903 20939 20957 20989 21372 21514 21529 21538 21542 21557 21586 21648 21671 21679 21683 21686 21719 22020 22044 22064 22068-22069 22071 22074 22106 22111 22116 22122 22130 22149 22169 22210 22214 22216 22219 22221 22223 22227 22239 22255 22267 22433 22438 22499 22871 22887 23538 23612 23622 23635 23660 23662 23669-23670 23745 23761-23762 23778 23816 23841 23846 23852 23861 23922 24002 24121 24146 24153 24226 24326 24330 24344 24411 24450 24453 24478-24479 24491 24522 24527 24544 24551 28711 28717 28779 28806 28808 28819 28893 28916 28991 29032 29066 29081 29089 29095 29104 29110 29126 29166 29216 29519 29523 29533 29665 29772 29852 29875 29897 29999 30128 30211 30219 30222-30223 30235 30245 30258 30265 30307 30311 30321-30322 30333 30438 30504 30580 30596 30609 30641 30646 32012 32064 32074 33099 33804 37203 37223 37235 37273 37303 37330 37332 37334 37336 37339-37340 37357 37364 37366 37674 37713 37721 37723 37729 37741 37745-37746 37757 37828-37829 37856 37867 37870 37888 37895 37903-37904 37915 37917 37923 37926-37927 37938 37963 37971 38020 38022-38024 38026 38029 38049 38242 38627 39125 39131 39216-39217 39231-39232 39244-39245 39348 39356 39374 39410 39766 39771 39790 39796 39883 39886 39889 39892 39920 39926 39933 39935 40580 40608 40696 41375 41383 41385 41419 41461 41556 41605 41608 41613 41681 41697-41698 41721-41722 41737 41761-41762 41810 41813 41834 41842 41860 41862 42153 42177 42185 42216 42274 42297 42352 42378 42402 42820 43013 43022 43028 43041 43047 43056-43057 43060https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/566/A37?format=asciiOpticaldefaultJ/A+A/566/A37/table3Mean NIR magnitudes, mean distances and mean iron abundances for the current sample of classical CepheidsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameVariable namemeta.id;meta.maincharVTypeVariable type (from GCVS) (1)meta.code;src.varcharlogPerlogarithmic periodlog(d)time.periodfloat<Jmag>Mean J magnitudemagphot.mag;em.IR.Jfloat<Hmag>Mean H magnitudemagphot.mag;em.IR.Hfloat<Kmag>Mean K magnitudemagphot.mag;em.IR.Kfloat[Fe/H]lIron abundance available in the literature rescaled to our solar abundancelog(Sun)phys.abund.Fefloat[Fe/H]Current iron abundancelog(Sun)phys.abund.Fefloate_[Fe/H]? rms uncertainty on [Fe/H] (only in table3)log(Sun)stat.error;phys.abund.FefloatnullableNsp? Number of spectra used to estimate the mean iron abundance (only in table3)meta.numberintnullableModTrue distance modulusmagphot.mag.distModfloate_Modrms uncertainty on Modmagstat.errorfloatRgalGalactocentric distance (R{sun}=7.95+/-0.37kpc)pcpos.distance;pos.galactocentricinte_Rgalrms uncertainty on Rgalpcstat.error;pos.distance;pos.galactocentricintNotesNotes on the NIR photometry and distances for individual objects (2)meta.notecharRefReferences (3)meta.refcharSimbadSimbad column added by the CDSmeta.ref.urlchar_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.mainJ/A+A/566/A37/table4Galactic Cepheids for which the iron abundance was available in the literaturelogPerlogarithmic periodlog(d)time.periodfloat<Jmag>Mean J magnitudemagphot.mag;em.IR.Jfloat<Hmag>Mean H magnitudemagphot.mag;em.IR.Hfloat<Kmag>Mean K magnitudemagphot.mag;em.IR.KfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameVariable namemeta.id;meta.maincharVTypeVariable type (from GCVS) (1)meta.code;src.varchar[Fe/H]lIron abundance available in the literature rescaled to our solar abundancelog(Sun)phys.abund.Fefloat[Fe/H]Current iron abundancelog(Sun)phys.abund.Fefloate_[Fe/H]? rms uncertainty on [Fe/H] (only in table3)log(Sun)stat.error;phys.abund.FefloatnullableNsp? Number of spectra used to estimate the mean iron abundance (only in table3)meta.numberintnullableModTrue distance modulusmagphot.mag.distModfloate_Modrms uncertainty on Modmagstat.errorfloatRgalGalactocentric distance (R{sun}=7.95+/-0.37kpc)pcpos.distance;pos.galactocentricinte_Rgalrms uncertainty on Rgalpcstat.error;pos.distance;pos.galactocentricintNotesNotes on the NIR photometry and distances for individual objects (2)meta.notecharRefReferences (3)meta.refcharSimbadSimbad column added by the CDSmeta.ref.urlchar_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.mainJ/A+A/566/A37/table5Individual ages, distances, and metallicities for the current sample of 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.maincharAgeCluster ageGyrtime.agefloatr_AgeReference for age-dist (1)meta.ref;pos.framecharRgalGalactocentric distance (R{sun}=7.94+/-0.37kpc)kpcpos.distance;pos.galactocentricfloat[Fe/H]lIron abundance available in the literaturelog(Sun)phys.abund.Fefloatr_[Fe/H]lReference for metallicitymeta.ref;pos.framechar[Fe/H]rMetallicity rescaled to current solar abundancelog(Sun)phys.abund.Zfloat_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.mainJ/A+A/566/A37/table6Structural parameters and metallicities of the candidate Cepheid groupsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDCepheid group identification number (I to X)meta.id;meta.mainnullableXGalactic coordinate X of the group barycenterkpcpos.cartesian.xfloatYGalactic coordinate Y of the group barycenterkpcpos.cartesian.y;pos.barycenter;pos.lgfloatZGalactic coordinate Z of the group barycenterkpcsrc.redshiftfloatRgalGalactocentric radius of the group barycenterkpcpos.distance;pos.galactocentricfloatdRgal-Galactocentric distance of the inner edge of the Cepheid groupkpcpos.distance;pos.galactocentricfloatdRgal+Galactocentric distance of the outer edge of the Cepheid groupkpcpos.distance;pos.galactocentricfloatDiamDiameter of the Cepheid groupkpcpos.distancefloatN[6/52] Number of Cepheids per Cepheid groupmeta.numberintPer[5.08/8.74] Mean period of Cepheids in groupdtime.period;stat.meanfloate_PerIntrinsic dispersion of Perdstat.errorfloatrhoDensity of tje Cepheid groupkpc**-3phys.densityfloatD[Fe/H]Mean residual iron abundance {Delta}[Fe/H]log(Sun)phys.abund.Fefloate_D[Fe/H]Intrinsic dispersion {sigma}({Delta}[Fe/H])log(Sun)stat.error;phys.abund.Fefloat