J/AJ/144/95ivo://CDS.VizieR/J/AJ/144/95doi:10.26093/cds/vizier.51440095CDSYong D.Carney B.W.Friel E.D.2017-12-07T07:27:16Z2013-11-29T07:32:15ZCDS support team

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

cds-question@unistra.fropen-star-clusterschemical-abundancesline-intensitiesextinctioneffective-temperatureinfrared-photometryvisible-astronomybroad-band-photometryinterstellar-reddeningWe present radial velocities and chemical abundances for nine stars in the old, distant open clusters Be18, Be21, Be22, Be32, and PWM4. For Be18 and PWM4, these are the first chemical abundance measurements. Combining our data with literature results produces a compilation of some 68 chemical abundance measurements in 49 unique clusters. For this combined sample, we study the chemical abundances of open clusters as a function of distance, age, and metallicity. We confirm that the metallicity gradient in the outer disk is flatter than the gradient in the vicinity of the solar neighborhood. We also confirm that the open clusters in the outer disk are metal-poor with enhancements in the ratios [{alpha}/Fe] and perhaps [Eu/Fe]. All elements show negligible or small trends between [X/Fe] and distance (<0.02dex/kpc), but for some elements, there is a hint that the local (R_GC_<13kpc) and distant (R_GC_>13kpc) samples may have different trends with distance. There is no evidence for significant abundance trends versus age (<0.04dex/Gyr). We measure the linear relation between [X/Fe] and metallicity, [Fe/H], and find that the scatter about the mean trend is comparable to the measurement uncertainties. Comparison with solar neighborhood field giants shows that the open clusters share similar abundance ratios [X/Fe] at a given metallicity. While the flattening of the metallicity gradient and enhanced [{alpha}/Fe] ratios in the outer disk suggest a chemical enrichment history different from that of the solar neighborhood, we echo the sentiments expressed by Friel et al. that definitive conclusions await homogeneous analyses of larger samples of stars in larger numbers of clusters. Arguably, our understanding of the evolution of the outer disk from open clusters is currently limited by systematic abundance differences between various studies.2012AJ....144...95Yhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/144/95CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toVII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)J/A+A/535/A30 : Abundance of 12 stars in open clusters (Carrera+, 2011)J/AJ/142/59 : Chemical abundance in 10 open clusters (Jacobson+, 2011)J/AJ/141/58 : NGC 2204 and NGC 2243 red giant abundances (Jacobson+, 2011)J/ApJ/735/L46 : Spectroscopy of 64 K red giants (Bensby+, 2011)J/AJ/139/1942 : EWs of red giants in 6 open clusters (Friel+, 2010)J/A+A/511/A56 : Abundances of five open clusters (Pancino+, 2010)J/AJ/137/4753 : Red giants EWs in 4 open clusters (Jacobson+, 2009)J/A+A/480/79 : Abundances of giants in 5 Galactic clustersJ/A+A/488/943 : Abundances of giants in 4 Galactic clusters (Sestito+, 2008)J/A+A/476/217 : Fundamental parameters of 5 old open clustersJ/A+A/465/185 : Element abundances of 7 stars of NGC 6253 (Sestito+, 2007)J/MNRAS/368/471 : Berkeley 32 BVI photometry and spectroscopy (D'Orazi+, 2006)J/AJ/130/1111 : Abundances of field red giants (Carney+, 2005, Paper II)J/AJ/129/2725 : Equivalent widths of red giants in Berkeley 17 (Friel+, 2005)J/A+A/431/933 : Abundances of NGC 7789 evolved stars (Tautvaisiene+, 2005)J/AJ/130/652 : EWs of 4 giants in Be22 and Be66 (Villanova+, 2005)J/AJ/129/656 : Infrared photometry of NGC 6791 (Carney+, 2005)J/A+A/423/199 : Chemical abundances of planetary nebulae (Costa+, 2004)J/A+A/392/491 : Galactic abundance gradient. III. (Andrievsky+, 2002)J/MNRAS/299/834 : Berkeley 21 BVI photometry (Tosi+, 1998)J/A+AS/121/455 : BVI photometry of stars in Berkeley 18 (Kaluzny 1997)J/A+AS/108/151 : Open clusters CCD photometry. I. (Kaluzny, 1994)J/AcA/41/167 : UBV photometry in Berkeley 32 (Kaluzny+, 1991)http://www.univie.ac.at/webda/ : WEBDA databasehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/144/95https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/144/95http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/144/95https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/144/95https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/144/95http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/144/95GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/144/95/table2 (Photometric data)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/144/95/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/144/95/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/144/95/table2?GETtext/xml+votable180.050000true80.55708345.4296670.0055555555555555566/1481 14303 22239 23612 243303.322582951404819e-19 3.852589004194616e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/144/95?format=asciiOpticalInfrareddefaultJ/AJ/144/95/table2Photometric dataSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar namemeta.id;meta.maincharprimaryNameName used as column header in table6 (equivalent widths)meta.idcharRAJ20002MASS Hour of Right Ascension (J2000)pos.eq.ra;meta.mainDEJ20002MASS Degree of Declination (J2000)pos.eq.dec;meta.mainVmag? The V band magnitudemagphot.mag;em.opt.VfloatnullableB-V? The B-V color indexmagphot.color;em.opt.B;em.opt.VfloatnullableV-Ic? The (V-I_C_) color indexmagphot.color;em.opt.V;em.opt.IfloatnullableKmag2MASS K band magnitudemagphot.mag;em.IR.KfloatJ-K2MASS (J-K) color indexmagphot.color;em.IR.J;em.IR.KfloatRef? Reference (1)meta.ref;pos.frameintnullable2MDisplay the 2MASS data (Cutri et al. 2003, Cat. II/246)meta.ref.urlcharJ/AJ/144/95/table4Red clump datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClusterCluster namemeta.id;meta.mainchar<Kmag>Mean K magnitudemagphot.mag;em.IR.Kfloat<J-K>Mean (J-K) color indexmagphot.color;em.IR.J;em.IR.Kfloat[Fe/H]Metallicity from our spectroscopic measurementlog(Sun)phys.abund.Zfloat(J-K)0(J-K)_0_magphot.color;em.IR.J;em.IR.KfloatE(J-K)Reddening E(J-K) [=0.52E(B-V)]. See section 2.4 for more detailsmagphot.color.excessfloatE(B-V)Estimated reddeningmagphot.color.excessfloat(m-M)0Distance modulus (m-M)_0_magphot.mag.distModfloatDistEstimated distancekpcpos.distance;pos.heliocentricfloatRgcGalactocentric distance R_GC_kpcpos.distance;pos.galactocentricfloatRedReddening from the WEBDA database (1)magphot.color.excessfloatdDistance from the WEBDA database (1)kpcpos.distance;pos.heliocentricfloatSimbadSimbad column added by the CDSmeta.refcharJ/AJ/144/95/table5Atmospheric parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar namemeta.id;meta.maincharTeff1Photometric effective temperature (1)Kphys.temperature.effectiveintlogg1Photometric surface gravity (1)log(cm.s**-2)phys.gravityfloatTeff2Photometric effective temperature (2)Kphys.temperature.effectiveintlogg2Photometric surface gravity (2)log(cm.s**-2)phys.gravityfloatTeff3Spectroscopic effective temperature (3)Kphys.temperature.effectiveintlogg3Spectroscopic surface gravity (3)log(cm.s**-2)phys.gravityfloat[m/H]Spectroscopic metallicity of the model (3)log(Sun)phys.abund.FefloatxiSpectroscopic microturbulent velocity ({xi}_t_) (3)km/sphys.veloc;pos.parallax.spectfloat[Fe/H]Spectroscopic derived metallicity (3)log(Sun)phys.abund.ZfloatJ/AJ/144/95/table6Equivalent widths for program starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[4439.88/8075.15] Wavelength; in {AA}0.1nmem.wlfloatIonAtomic element and ionization numberphys.atmol.ionStagefloatLEPLower excitation potentialeVphys.atmol.excitation;stat.minfloatloggfLog of the oscillator strengthphys.atmol.oscStrengthfloatE1163? Be18-1163 equivalent width; in m{AA}1e-13mspect.line.widthfloatnullableE1383? Be18-1383 equivalent width; in m{AA}1e-13mspect.line.widthfloatnullableET50? Be21-T50 equivalent width; in m{AA}1e-13mspect.line.eqWidthfloatnullableET51? Be21-T51 equivalent width; in m{AA}1e-13mspect.line.eqWidthfloatnullableE414? Be22-414 equivalent width; in m{AA}1e-13mspect.line.widthfloatnullableE643? Be22-643 equivalent width; in m{AA}1e-13mspect.line.widthfloatnullableE16? Be32-16 equivalent width; in m{AA}1e-13mspect.line.widthfloatnullableE18? Be32-18 equivalent width; in m{AA}1e-13mspect.line.widthfloatnullableERGB1? PWM-RGB1 equivalent width; in m{AA}1e-13mspect.line.eqWidthfloatnullableJ/AJ/144/95/abundChemical abundances for the program stars (tables 7-11)StarStar namemeta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonSpeciesphys.atmol.ionStagechar[X/Fe]? Chemical abundance ratiolog(Sun)phys.abundfloatnullablee_[X/Fe]? sigma uncertainty in [X/Fe]log(Sun)stat.error;phys.abundfloatnullableN? Number of linesmeta.numberintnullableJ/AJ/144/95/table13Compilation of (LTE) abundance ratios for open clustersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClusterCluster namemeta.id;meta.maincharr_AgeSource reference (1)meta.ref;pos.framecharAge? Age from the individual papersGyrtime.agefloatnullablef_AgeFlag on Age (c = age from Bragaglia & Tosi, 2006AJ....131.1544B)meta.codecharDist? Galactocentric distance from the individual paperskpcpos.distancefloatnullablef_DistFlag on Dist (c = distance from Bragaglia & Tosi, 2006AJ....131.1544B)meta.codecharAge2? Age from Salaris et al. (2004A&A...414..163S)Gyrtime.agefloatnullableDist2? Galactocentric distance (from Salaris et al., 2004A&A...414..163S)kpcpos.distance;pos.galactocentricfloatnullable[Fe/H]The [Fe/H] number abundancemeta.idfloat[O/Fe]? The [O/Fe] number abundancemeta.idfloatnullable[Na/Fe]? The [Na/Fe] number abundancemeta.idfloatnullable[Mg/Fe]? The [Mg/Fe] number abundancemeta.idfloatnullable[Al/Fe]? The [Al/Fe] number abundancemeta.idfloatnullable[Si/Fe]? The [Si/Fe] number abundancemeta.idfloatnullable[Ca/Fe]? The [Ca/Fe] number abundancemeta.idfloatnullable[Ti/Fe]? The [Ti/Fe] number abundancemeta.idfloatnullable[Mn/Fe]? The [Mn/Fe] number abundancemeta.idfloatnullable[Co/Fe]? The [Co/Fe] number abundancemeta.idfloatnullable[Ni/Fe]? The [Ni/Fe] number abundancemeta.idfloatnullable[Zr/Fe]? The [Zr/Fe] number abundancemeta.idfloatnullable[Ba/Fe]? The [Ba/Fe] number abundancemeta.idfloatnullable[La/Fe]? The [La/Fe] number abundancemeta.idfloatnullable[Eu/Fe]? The [Eu/Fe] number abundancemeta.idfloatnullableJ/AJ/144/95/table14Mean [X/Fe] ratios, standard error of the mean, and level of significance when comparing the inner and outer disks for different boundary valuesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonSpeciesphys.atmol.ionStagecharAb10iMean [X/Fe] ratio in the inner disk for a boundary value of R_GC_=10kpcphys.abundfloate_Ab10iStandard error in Ab10istat.errorfloatAb10oMean [X/Fe] ratio in the outer disk for a boundary value of R_GC_=10kpcphys.abundfloate_Ab10oStandard error in Ab10ostat.errorfloatSig10Level of significance (see Section 4.1 for more details) for a boundary value of R_GC_=10kpcstat.fit.goodnessfloatAb13iMean [X/Fe] ratio in the inner disk for a boundary value of R_GC_=13kpcphys.abundfloate_Ab13iStandard error in Ab13istat.errorfloatAb13oMean [X/Fe] ratio in the outer disk for a boundary value of R_GC_=13kpcphys.abundfloate_Ab13oStandard error in Ab13ostat.errorfloatSig13Level of significance (see Section 4.1 for more details) for a boundary value of R_GC_=13kpcstat.fit.goodnessfloatAb15iMean [X/Fe] ratio in the inner disk for a boundary value of R_GC_=15kpcphys.abundfloate_Ab15iStandard error in Ab15istat.errorfloatAb15oMean [X/Fe] ratio in the outer disk for a boundary value of R_GC_=15kpcphys.abundfloate_Ab15oStandard error in Ab15ostat.errorfloatSig15Level of significance (see Section 4.1 for more details) for a boundary value of R_GC_=15kpcstat.fit.goodnessfloat