J/A+A/533/A134ivo://CDS.VizieR/J/A+A/533/A134doi:10.26093/cds/vizier.35330134CDSBensbyT.AdenD.MelendezJ.GouldA.FeltzingS.,AsplundM.JohnsonJ.A.LucatelloS.YeeJ.C.RamirezI.,CohenJ.G.ThompsonI.Gal-YamA.Han C.SumiT.Suzuki D.,Wada K.Miyake N.Furusawa K.Ohmori K.Saito To.Tristram P.,Bennett D.2017-07-05T07:00:19Z2011-09-15T08:20:55ZCDS support team

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

cds-question@unistra.frgravitational-lensingchemical-abundancesline-intensitiesWe perform a detailed elemental abundance analysis of dwarf stars in the Galactic bulge, based on high-resolution spectra that were obtained while the stars were optically magnified during gravitational microlensing events. The analysis method is the same as for a large sample of F and G dwarf stars in the Solar neighbourhood, enabling a fully differential comparison between the Bulge and the local stellar populations in the Galactic disc.2011A&A...533A.134Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/533/A134CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/415/155 : Oxygen abundances in the Galactic disk (Bensby+, 2004)J/A+A/499/737 : Abundances of microlensed dwarf & subgiant stars (Bensby+ 2009)J/A+A/512/A41 : Abundances of microlensed stars in the Bulge (Bensby+, 2010)J/A+A/512/A54 : Teff and Fbol from Infrared Flux Method (Casagrande+, 2010)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/533/A134https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/533/A134http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/533/A134https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/533/A134https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/533/A134http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/533/A134GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/533/A134/stars (Results of the twelve microlensing events in the Bulge presented, including stellar parameters, radial velocities, and abundances)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/533/A134/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/533/A134/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/533/A134/stars?GETtext/xml+votable180.050000true270.5320833-31.4240.0055555555555555566/28733 28780 28783 28821-28822 28864 28868 28871 28882https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/533/A134?format=asciiOpticaldefaultJ/A+A/533/A134/starsResults of the twelve microlensing events in the Bulge presented, including stellar parameters, radial velocities, and abundances[Ti/Fe]Normalised abundancelog(Sun)phys.abundfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar namemeta.id;meta.maincharAbDetailed equivalent widths and abundances for this star from table5meta.ref.urlcharT3Display ages and atmopshpeiric parameters from other sourcesmeta.ref.urlcharGLON[-90/90] Galactic longitudedegpos.galactic.lonGLATGalactic latitudedegpos.galactic.latfloatDt? Duration of the eventdtime.durationintnullablet.maxTime when maximum magnification occured (HJD-2450000)dtime.epochdoubleAmax? Maximum magnificationphot.mag;arith.ratiointnullablet.obsTime when event was observed with high-resolution spectrograph (MJD)dtime.epochdoublet.expExposure timestime.duration;obs.exposureintS/NMeasured signal-to-noise ratio per pixel at ~6400{AA}stat.snr;instr.pixelintSpecSpectrograph usedmeta.id;instrcharRSpectral resolutionspect.resolutionintTeffEffective temperatureKphys.temperature.effectiveinte_Teffrms uncertainty on TeffKstat.error;phys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloate_loggrms uncertainty on logglog(cm.s**-2)stat.errorfloatvtMicroturbulence parameterkm/sstat.paramfloate_vtrms uncertainty on vtkm/sstat.errorfloat[Fe/H]Metallicitylog(Sun)phys.abund.Zfloate_[Fe/H]rms uncertainty on [Fe/H]log(Sun)stat.error;phys.abund.Fefloatn(FeI)Number of FeI lines used in the analysismeta.numberintn(FeII)Number of FeII lines used in the analysismeta.numberintRVRadial velocitykm/sphys.veloc;pos.heliocentricfloat[O/Fe]Normalised abundance (not NLTE corrected)log(Sun)phys.abundfloate_[O/Fe]? Error in abundance ratiolog(Sun)phys.abundfloatnullable[Na/Fe]Normalised abundancelog(Sun)phys.abundfloate_[Na/Fe]? Error in abundance ratiolog(Sun)phys.abundfloatnullable[Mg/Fe]Normalised abundancelog(Sun)phys.abundfloate_[Mg/Fe]? Error in abundance ratiolog(Sun)phys.abundfloatnullable[Al/Fe]Normalised abundancelog(Sun)phys.abundfloate_[Al/Fe]? Error in abundance ratiolog(Sun)phys.abundfloatnullable[Si/Fe]Normalised abundancelog(Sun)phys.abundfloate_[Si/Fe]? Error in abundance ratiolog(Sun)phys.abundfloatnullable[Ca/Fe]Normalised abundancelog(Sun)phys.abundfloate_[Ca/Fe]? Error in abundance ratiolog(Sun)phys.abundfloatnullablee_[Ti/Fe]? Error in abundance ratiolog(Sun)phys.abundfloatnullable[Cr/Fe]? Normalised abundancelog(Sun)phys.abundfloatnullablee_[Cr/Fe]? Error in abundance ratiolog(Sun)phys.abundfloatnullable[Ni/Fe]Normalised abundancelog(Sun)phys.abundfloate_[Ni/Fe]? Error in abundance ratiolog(Sun)phys.abundfloatnullable[Zn/Fe]? Normalised abundancelog(Sun)phys.abundfloatnullablee_[Zn/Fe]? Error in abundance ratiolog(Sun)phys.abundfloatnullable[Y/Fe]? Normalised abundancelog(Sun)phys.abundfloatnullablee_[Y/Fe]? Error in abundance ratiolog(Sun)phys.abundfloatnullable[Ba/Fe]Normalised abundancelog(Sun)phys.abundfloate_[Ba/Fe]? Error in abundance ratiolog(Sun)phys.abundfloatnullablen(Fe)? Number of Fe lines usedmeta.numberintnullablen(O)? Number of O lines usedmeta.numberintnullablen(Na)? Number of Na lines usedmeta.numberintnullablen(Mg)? Number of Mg lines usedmeta.numberintnullablen(Al)? Number of Al lines usedmeta.numberintnullablen(Si)? Number of Si lines usedmeta.numberintnullablen(Ca)? Number of Ca lines usedmeta.numberintnullablen(Ti)? Number of Ti lines usedmeta.numberintnullablen(Cr)? Number of Cr lines usedmeta.numberintnullablen(Ni)? Number of Ni lines usedmeta.numberintnullablen(Zn)? Number of Zn lines usedmeta.numberintnullablen(Y)? Number of Y lines usedmeta.numberintnullablen(Ba)? Number of Ba lines usedmeta.numberintnullableRAJ2000Right ascension (J2000) (1)pos.eq.ra;meta.mainDEJ2000Declination (J2000) (1)pos.eq.dec;meta.mainJ/A+A/533/A134/table3*Stellar ages and a comparison of colours and effective temperatures as determined from spectroscopy and microlensing techniques for all 26 microlensed dwarf starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameObject namemeta.id;meta.maincharTeffEffective temperatureKphys.temperature.effectiveintMStellar mass (inferred from isochrones)solMassphys.massfloatlogLLuminosity (inferred from isochrones)log(solLum)phys.luminosityfloatAgeAge (inferred from isochrones)Gyrtime.agefloatb_Age1-sigma lower estimate of AgeGyrtime.age;stat.minfloatB_Age1-sigma upper estimate of AgeGyrtime.age;stat.maxfloat(V-I)0Deredenned V-I colour index (1)magphot.color;em.opt.V;em.opt.IfloatVMAGAbsolute V magnitude based on the spectroscopic stellar parametersmagphys.magAbs;em.opt.Vfloatb_VMAG1-sigma lower estimate of VMAGmagphys.magAbs;em.opt.V;stat.minfloatB_VMAG1-sigma upper estimate of VMAGmagphys.magAbs;em.opt.V;stat.maxfloatIMAG? Absolute I magnitude based on spectroscopic stellar parametersmagphys.magAbs;em.opt.IfloatnullableIMAGm? Absolute I magnitude (based on microlensing technique)magphys.magAbsfloatnullable(V-I)0m? Deredenned V-I colour index (based on microlensing technique)magphot.color;em.opt.V;em.opt.IfloatnullableTeffm? Inferred effective temperature (based on microlensing technique) (1)Kphys.temperature.effectiveintnullableComComments ("DR" = for differential reddening)meta.notecharJ/A+A/533/A134/table5Equivalent widths and absolute abundances for individual linesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElElementphys.atmol.elementcharIonIonisation (1=neutral)phys.atmol.ionStageintlambdaWavelength0.1nmem.wldoubleLEPLower Excitation PotentialeVphys.atmol.excitation;stat.minfloatWsunEquivalent width Sun0.1pmspect.line.eqWidthfloatA(Sun)Sun absolute abundance (log scale, A(H)=12)phys.abundfloatf_A(Sun)[0,1] 0 if line measured and used, 1 if average abundance from other lines usedmeta.codeintW(174S)? Equivalent width MOA-2009-BLG-174S0.1pmspect.line.eqWidthfloatnullableA(174S)? Absolute abundance MOA-2009-BLG-174Sphys.abundfloatnullableW(259S)? Equivalent width MOA-2009-BLG-259S0.1pmspect.line.eqWidthfloatnullableA(259S)? Absolute abundance MOA-2009-BLG-259Sphys.abundfloatnullableW(037S)? Equivalent width MOA-2010-BLG-037S0.1pmspect.line.eqWidthfloatnullableA(037S)? Absolute abundance MOA-2010-BLG-037Sphys.abundfloatnullableW(049S)? Equivalent width MOA-2010-BLG-049S0.1pmspect.line.eqWidthfloatnullableA(049S)? Absolute abundance MOA-2010-BLG-049Sphys.abundfloatnullableW(078S)? Equivalent width MOA-2010-BLG-078S0.1pmspect.line.eqWidthfloatnullableA(078S)? Absolute abundance MOA-2010-BLG-078Sphys.abundfloatnullableW(167S)? Equivalent width MOA-2010-BLG-167S0.1pmspect.line.eqWidthfloatnullableA(167S)? Absolute abundance MOA-2010-BLG-167Sphys.abundfloatnullableW(285S)? Equivalent width MOA-2010-BLG-285S0.1pmspect.line.eqWidthfloatnullableA(285S)? Absolute abundance MOA-2010-BLG-285Sphys.abundfloatnullableW(311S)? Equivalent width MOA-2010-BLG-311S0.1pmspect.line.eqWidthfloatnullableA(311S)? Absolute abundance MOA-2010-BLG-311Sphys.abundfloatnullableW(446S)? Equivalent width MOA-2010-BLG-446S0.1pmspect.line.eqWidthfloatnullableA(446S)? Absolute abundance MOA-2010-BLG-446Sphys.abundfloatnullableW(523S)? Equivalent width MOA-2010-BLG-523S0.1pmspect.line.eqWidthfloatnullableA(523S)? Absolute abundance MOA-2010-BLG-523Sphys.abundfloatnullableW(034S)? Equivalent width MOA-2011-BLG-034S0.1pmspect.line.eqWidthfloatnullableA(034S)? Absolute abundance MOA-2011-BLG-034Sphys.abundfloatnullableW(058S)? Equivalent width MOA-2011-BLG-058S0.1pmspect.line.eqWidthfloatnullableA(058S)? Absolute abundance MOA-2011-BLG-058Sphys.abundfloatnullable