J/ApJ/746/29ivo://CDS.VizieR/J/ApJ/746/29doi:10.26093/cds/vizier.17460029CDSColucci J.E.Bernstein R.A.Cameron S.A.McWilliam A.2018-01-11T12:51:12Z2013-09-12T13:24:16ZCDS support team

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

cds-question@unistra.frglobular-star-clustersmagellanic-cloudschemical-abundancesline-intensitiesWe present detailed chemical abundances in eight clusters in the Large Magellanic Cloud (LMC). We measure abundances of 22 elements for clusters spanning a range in age of 0.05-12 Gyr, providing a comprehensive picture of the chemical enrichment and star formation history of the LMC. The abundances were obtained from individual absorption lines using a new method for analysis of high-resolution (R~25000), integrated-light (IL) spectra of star clusters. This method was developed and presented in Papers I (2008ApJ...684..326M), II (2009PhDT........20C), and III (Cat. J/ApJ/735/55) of this series. In this paper, we develop an additional IL {chi}^2^-minimization spectral synthesis technique to facilitate measurement of weak (~15m{AA}) spectral lines and abundances in low signal-to-noise ratio data (S/N~30). Additionally, we supplement the IL abundance measurements with detailed abundances that we measure for individual stars in the youngest clusters (age<2Gyr) in our sample. In both the IL and stellar abundances we find evolution of [{alpha}/Fe] with [Fe/H] and age. Fe-peak abundance ratios are similar to those in the Milky Way (MW), with the exception of [Cu/Fe] and [Mn/Fe], which are sub-solar at high metallicities. The heavy elements Ba, La, Nd, Sm, and Eu are significantly enhanced in the youngest clusters. Also, the heavy to light s-process ratio is elevated relative to the MW ([Ba/Y]>+0.5) and increases with decreasing age, indicating a strong contribution of low-metallicity asymptotic giant branch star ejecta to the interstellar medium throughout the later history of the LMC. We also find a correlation of IL Na and Al abundances with cluster mass in the sense that more massive, older clusters are enriched in the light elements Na and Al with respect to Fe, which implies that these clusters harbor star-to-star abundance variations as is common in the MW. Lower mass, intermediate-age, and young clusters have Na and Al abundances that are lower and more consistent with LMC field stars. Our results can be used to constrain both future chemical evolution models for the LMC and theories of globular cluster formation.2012ApJ...746...29Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/746/29CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJ/735/55 : High-resolution GCs abundances. III. LMC (Colucci+, 2011)J/A+A/536/A60 : EROS-2 Long Period Variables in LMC (Spano+, 2011)J/ApJ/717/277 : Chemical composition of old LMC clusters (Mucciarelli+, 2010)J/ApJ/695/L134 : Chemical anomalies in old LMC clusters (Mucciarelli+, 2009)J/ApJ/704/385 : M31 integrated light abundances (Colucci+, 2009)J/AJ/136/375 : Chemical composition of LMC red giants (Mucciarelli+, 2008)J/A+A/480/379 : Abundances of 59 red giants in LMC (Pompeia+, 2008)J/ApJS/155/401 : Magellanic clouds GCs ISOCAM obs. (Tanabe+, 2004)J/A+A/293/347 : LMC F supergiants (Hill+, 1995)J/MNRAS/260/782 : CCD photometry of NGC 2004 and 2100 (Balona+ 1993)J/ApJS/71/25 : NGC 1866 CCD photometry (Brocato+ 1989)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/746/29https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/746/29http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/746/29https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/746/29https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/746/29http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/746/29GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/746/29/table1 (LMC cluster properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/746/29/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/746/29/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/746/29/table1?GETtext/xml+votable180.050000true79.657792-69.4063610.005555555555555556Cone search capability for table J/ApJ/746/29/stars (Stellar targets from table 1 of 2012ApJ...749..124C)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/746/29/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/746/29/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/746/29/stars?GETtext/xml+votable180.050000true82.17996-66.208390.0055555555555555566/33075 33078 33094 33096 33097 33098 33113 33123 33137https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/746/29?format=asciidefaultJ/ApJ/746/29/table1LMC cluster propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClassOld(>5Gyr), Int(1-3Gyr), or Yng(<1Gyr)src.classcharNGCCluster NGC numbermeta.id;meta.mainintl_AgeLimit flag on Agemeta.code.error;time.agecharAgeAge limit or rangeGyrtime.agefloatB_Age? Upper age rangeGyrtime.age;stat.maxfloatnullable[Fe/H]Metallicitylog(Sun)phys.abund.ZfloatB_[Fe/H]? Upper metallicity range (if filled, Metallicity is the lower range)log(Sun)phys.abund.Z;stat.maxfloatnullablee_[Fe/H]? Uncertainty in [Fe/H]log(Sun)stat.error;phys.abund.Fefloatnullable[a/Fe]? Mean abundance of {alpha} elements (1)log(Sun)phys.abundfloatnullable[a/Fe]2? Second value of [a/Fe] (1)log(Sun)phys.abundfloatnullableRefReference(s) (2)meta.ref;pos.framecharEWDisplay the equivalent width data for this cluster (table 2)meta.ref.urlcharSimbadSimbad column added by the CDSmeta.ref.urlchar_RAPositions from SIMBAD database (right ascension part)degpos.eq.ra;meta.main_DEPositions from SIMBAD database (declination part)degpos.eq.dec;meta.mainJ/ApJ/746/29/starsStellar targets from table 1 of 2012ApJ...749..124CSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar designationmeta.id;meta.maincharRAJ2000Right ascension in decimal degrees (J2000)degpos.eq.ra;meta.mainDEJ2000Declination in decimal degrees (J2000)degpos.eq.dec;meta.mainObsYear of observationtime.epochEWDisplay the Equivalent Widths for this star from table3meta.ref.urlcharJ/ApJ/746/29/table2Line parameters and integrated-light equivalent widths for LMC GCsTypeMethod type (4)meta.notecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonSpecies identification (G1)phys.atmol.ionStagecharlambdaWavelength {lambda} (in Angstroms)0.1nmem.wldoubleExPotExcitation potential (G2)eVphys.atmol.excitationfloatlog(gf)Log of the oscillator strengthphys.atmol.oscStrengthfloatEW1916? Equivalent width for NGC 1916 (G3)1e-13mspect.line.eqWidthfloatnullableEW2005? Equivalent width for NGC 2005 (G3)1e-13mspect.line.eqWidthfloatnullableEW2019? Equivalent width for NGC 2019 (G3)1e-13mspect.line.eqWidthfloatnullableEW1978? Equivalent width for NGC 1978 (G3)1e-13mspect.line.eqWidthfloatnullableEW1718? Equivalent width for NGC 1718 (G3)1e-13mspect.line.eqWidthfloatnullableEW1866? Equivalent width for NGC 1866 (G3)1e-13mspect.line.eqWidthfloatnullableEW1711? Equivalent width for NGC 1711 (G3)1e-13mspect.line.eqWidthfloatnullableEW2100? Equivalent width for NGC 2100 (G3)1e-13mspect.line.eqWidthfloatnullableJ/ApJ/746/29/table3Line parameters and stellar equivalent widthsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonSpecies identification (G1)phys.atmol.ionStagecharlambdaWavelength {lambda} (in Angstroms)0.1nmem.wldoubleExPotExcitation potentialeVphys.atmol.excitationfloatlog(gf)Log of the oscillator strength (G2)phys.atmol.oscStrengthfloatEW1978-737? Equivalent width for star 1978-737 (G3)1e-13mspect.line.eqWidthfloatnullablef_EW1978-737[S] not used for abundance (4)meta.codecharEW1978-730? Equivalent width for star 1978-730 (G3)1e-13mspect.line.eqWidthfloatnullablef_EW1978-730[S] not used for abundance (4)meta.codecharEW1866-954? Equivalent width for star 1866-954 (G3)1e-13mspect.line.eqWidthfloatnullablef_EW1866-954[S] not used for abundance (4)meta.codecharEW1866-1653? Equivalent width for star 1866-1653(G3)1e-13mspect.line.eqWidthfloatnullablef_EW1866-1653[S] not used for abundance (4)meta.codecharEW1866-1667? Equivalent width for star 1866-1667(G3)1e-13mspect.line.eqWidthfloatnullablef_EW1866-1667[S] not used for abundance (4)meta.codecharEW1711-831? Equivalent width for star 1711-831 (G3)1e-13mspect.line.eqWidthfloatnullablef_EW1711-831[S] not used for abundance (4)meta.codecharEW1711-988? Equivalent width for star 1711-988 (G3)1e-13mspect.line.eqWidthfloatnullablef_EW1711-988[S] not used for abundance (4)meta.codecharEW1711-1194? Equivalent width for star 1711-1194 (G3)1e-13mspect.line.eqWidthfloatnullablef_EW1711-1194[S] not used for abundance (4)meta.codecharEW2100-c12? Equivalent width for star 2100-c12 (G3)1e-13mspect.line.eqWidthfloatnullablef_EW2100-c12[S] not used for abundance (4)meta.codecharEW2100-b22? Equivalent width for star 2100-b22 (G3)1e-13mspect.line.eqWidthfloatnullablef_EW2100-b22[S] not used for abundance (4)meta.codecharNote"HFS" for hyperfine splitting (5)meta.notechar