J/A+A/693/A163ivo://CDS.VizieR/J/A+A/693/A163doi:10.26093/cds/vizier.36930163CDSTaniguchi D.Matsunaga N.Kobayashi N.Jian M.Thorsbro B.Fukue K.,Hamano S.Ikeda Y.Kawakita H.Kondo S.Otsubo S.Sameshima H.,Tsujimoto T.Yasui C.2025-03-07T20:01:03Z2025-01-15T07:34:57ZCDS support team

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

cds-question@unistra.frsupergiant-starslate-type-starschemical-abundanceseffective-temperatureinfrared-astronomyspectroscopyRed supergiants (RSGs) are good tracers of chemical abundances of the young population in the Milky Way and nearby galaxies, given their high luminosities (L>~10^4^L{sun}_). However, previous abundance analysis methods for RSGs suffer some systematic uncertainties originating in, most notably, synthesized spectra for RSGs of molecular lines. We establish an abundance analysis procedure for RSGs to circumvent problems of previous works and test the procedure with ten nearby RSGs observed with the near-infrared high-resolution spectrograph WINERED (0.97-1.32 micron, R=28000). The wavelength range has an advantage that molecular lines contaminating atomic lines of interest are mostly weak. We first determine the effective temperatures (Teff) of the targets with the line-depth ratio (LDR) method, and calculate the surface gravities (logg) according to the Stefan-Boltzmann law. Then, we determine the microturbulent velocities (vmicro) and metallicities ([Fe/H]) simultaneously through the fitting of individual FeI lines. Finally, we determine the abundance ratios ([X/Fe] for element X) also through the fitting of individual lines. We determined [X/Fe] of ten elements (NaI, MgI, AlI, SiI, KI, CaI, TiI, CrI, NiI, and YII). We estimated the relative precision in the derived abundances to be 0.04-0.12dex for elements with more than two lines analyzed (e.g., FeI and MgI) and up to 0.18dex for the other elements (e.g., YII). We compared the resultant abundances of RSGs with the well-established abundances of another type of young stars, Cepheids, to evaluate the potential systematic bias in our abundance measurements, assuming that the young stars (i.e., both RSGs and Cepheids) in the solar neighborhood have common chemical abundances. Consequently, we found that the determined RSG abundances are well consistent with Cepheids within <~0.1dex for some elements (notably, [Fe/H] and [Mg/Fe]). In other words, the bias in the abundance determination for these elements would be small. In contrast, the consistency is worse for some other elements (e.g., [Si/Fe] and [Y/Fe]). Nevertheless, the dispersion of the chemical abundances among our target RSGs was comparable with the individual statistical errors of the abundances. Hence, the procedure would be useful for evaluating the relative difference in chemical abundances among RSGs.2025A&A...693A.163Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/693/A163CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/693/A163https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/693/A163http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/693/A163https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/693/A163https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/693/A163http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/693/A163GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapAssociated datahttps://cdsarc.cds.unistra.fr/assocdata/?obs_collection=J/A+A/693/A1637.952274030004205e-20 1.0188844282367877e-19InfrareddefaultJ/A+A/693/A163/table1Observation log and reduced spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of RSGmeta.id;meta.maincharHDHD numbermeta.idintSpTypeSpectral type (1)src.spTypecharObs.dateObservation datetime.epoch;obsnullableSpShow the spectrummeta.ref.urlcharFileNameName of spectrum in subdirectory sp (2)meta.idcharAssocDataAssociated Data web pagemeta.ref.urlcharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/A+A/693/A163/table2Derived logg and related valuesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of RSGmeta.id;meta.maincharplxParallax (1)maspos.parallax.trigfloate_plxError in plx (1)masstat.error;pos.parallaxfloatKsmagKs-band magnitude (2)magphot.mag;em.IR.Kfloate_KsmagError in Ksmag (2)magstat.error;phot.magfloatA(V)V-band extinction (3)magphys.absorptionfloate_A(V)Error in A(V) (3)magstat.errorfloatTeffEffective temperature (4)Kphys.temperature.effectiveinte_TeffError in Teff (4)Kstat.error;phys.temperature.effectiveintBCksKs-band bolometric correctionmagphot.mag.bcfloate_BCksError in BCksmagstat.errorfloatlogLLuminosity in log scalelog(solLum)phys.luminosityfloatb_logLLower confidence bound of logLlog(solLum)stat.fit.paramfloatB_logLUpper confidence bound of logLlog(solLum)stat.fit.paramfloatb_MassLower bound of current masssolMassphys.mass;stat.minintB_MassUpper bound of current masssolMassphys.mass;stat.maxintloggSurface gravity in log scale (4)log(cm.s**-2)instr.scalefloatb_loggLower confidence bound of logg (4)log(cm.s**-2)stat.fit.paramfloatB_loggUpper confidence bound of logg (4)log(cm.s**-2)stat.fit.paramfloatJ/A+A/693/A163/table3Derived stellar parameters and [Fe/H]vmic(V)Microturbulence determined with VALD3km/sphys.veloc.microTurbfloatb_vmic(V)Lower confidence bound of vmic(V)km/sstat.fit.paramfloatB_vmic(V)Upper confidence bound of vmic(V)km/sstat.fit.paramfloat[Fe/H](V)Metallicity determined with VALD3 (2)log(Sun)phys.abund.Fefloatb_[Fe/H](V)Lower confidence bound of [Fe/H](V) (2)log(Sun)phys.abund.FefloatB_[Fe/H](V)Upper confidence bound of [Fe/H](V) (2)log(Sun)phys.abund.Fefloatvmic(M)Microturbulence determined with MB99km/sphys.veloc.microTurbfloatb_vmic(M)Lower confidence bound of vmic(M)km/sstat.fit.paramfloatB_vmic(M)Upper confidence bound of vmic(M)km/sstat.fit.paramfloat[Fe/H](M)Metallicity determined with MB99 (2)log(Sun)phys.abund.FefloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of RSGmeta.id;meta.maincharTeffEffective temperature (1)Kphys.temperature.effectiveinte_TeffError in Teff (1)Kstat.error;phys.temperature.effectiveintloggSurface gravity in log scale (1)log(cm.s**-2)instr.scalefloatb_loggLower confidence bound of logg (1)log(cm.s**-2)stat.fit.paramfloatB_loggUpper confidence bound of logg (1)log(cm.s**-2)stat.fit.paramfloatb_[Fe/H](M)Lower confidence bound of [Fe/H](M) (2)log(Sun)phys.abund.FefloatB_[Fe/H](M)Upper confidence bound of [Fe/H](M) (2)log(Sun)phys.abund.FefloatJ/A+A/693/A163/table4aDerived chemical abundances [X/H]o_[Na/H]? Number of lines used for [Na/H] (3)meta.numberintnullable[Mg/H]? [Mg/H] abundancelog(Sun)phys.abundfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordint[Fe/H]Metallicity (2)log(Sun)phys.abund.Fefloatb_[Fe/H]Lower confidence bound of [Fe/H] (2)log(Sun)phys.abund.FefloatB_[Fe/H]Upper confidence bound of [Fe/H] (2)log(Sun)phys.abund.Fefloato_[Fe/H]Number of lines used for [Fe/H]meta.numberint[Na/H]? [Na/H] abundancelog(Sun)phys.abundfloatnullableb_[Na/H]? Lower confidence bound of [Na/H]log(Sun)stat.fit.paramfloatnullableB_[Na/H]? Upper confidence bound of [Na/H]log(Sun)stat.fit.paramfloatnullableb_[Mg/H]? Lower confidence bound of [Mg/H]log(Sun)stat.fit.paramfloatnullableB_[Mg/H]? Upper confidence bound of [Mg/H]log(Sun)stat.fit.paramfloatnullableo_[Mg/H]? Number of lines used for [Mg/H] (3)meta.numberintnullable[Al/H]? [Al/H] abundancelog(Sun)phys.abundfloatnullableb_[Al/H]? Lower confidence bound of [Al/H]log(Sun)stat.fit.paramfloatnullableB_[Al/H]? Upper confidence bound of [Al/H]log(Sun)stat.fit.paramfloatnullableo_[Al/H]? Number of lines used for [Al/H] (3)meta.numberintnullable[Si/H]? [Si/H] abundancelog(Sun)phys.abundfloatnullableb_[Si/H]? Lower confidence bound of [Si/H]log(Sun)stat.fit.paramfloatnullableB_[Si/H]? Upper confidence bound of [Si/H]log(Sun)stat.fit.paramfloatnullableo_[Si/H]? Number of lines used for [Si/H] (3)meta.numberintnullable[K/H]? [K/H] abundancelog(Sun)phys.abundfloatnullableb_[K/H]? Lower confidence bound of [K/H]log(Sun)stat.fit.paramfloatnullableB_[K/H]? Upper confidence bound of [K/H]log(Sun)stat.fit.paramfloatnullableo_[K/H]? Number of lines used for [K/H] (3)meta.numberintnullable[Ca/H]? [Ca/H] abundancelog(Sun)phys.abundfloatnullableb_[Ca/H]? Lower confidence bound of [Ca/H]log(Sun)stat.fit.paramfloatnullableB_[Ca/H]? Upper confidence bound of [Ca/H]log(Sun)stat.fit.paramfloatnullableo_[Ca/H]? Number of lines used for [Ca/H] (3)meta.numberintnullable[Ti/H]? [Ti/H] abundancelog(Sun)phys.abundfloatnullableb_[Ti/H]? Lower confidence bound of [Ti/H]log(Sun)stat.fit.paramfloatnullableB_[Ti/H]? Upper confidence bound of [Ti/H]log(Sun)stat.fit.paramfloatnullableo_[Ti/H]? Number of lines used for [Ti/H] (3)meta.numberintnullable[Cr/H]? [Cr/H] abundancelog(Sun)phys.abundfloatnullableb_[Cr/H]? Lower confidence bound of [Cr/H]log(Sun)stat.fit.paramfloatnullableB_[Cr/H]? Upper confidence bound of [Cr/H]log(Sun)stat.fit.paramfloatnullableo_[Cr/H]? Number of lines used for [Cr/H] (3)meta.numberintnullable[Ni/H]? [Ni/H] abundancelog(Sun)phys.abundfloatnullableb_[Ni/H]? Lower confidence bound of [Ni/H]log(Sun)stat.fit.paramfloatnullableB_[Ni/H]? Upper confidence bound of [Ni/H]log(Sun)stat.fit.paramfloatnullableo_[Ni/H]? Number of lines used for [Ni/H] (3)meta.numberintnullable[Y/H]? [Y/H] abundancelog(Sun)phys.abundfloatnullableb_[Y/H]? Lower confidence bound of [Y/H]log(Sun)stat.fit.paramfloatnullableB_[Y/H]? Upper confidence bound of [Y/H]log(Sun)stat.fit.paramfloatnullableo_[Y/H]? Number of lines used for [Y/H] (3)meta.numberintnullableNameName of RSGmeta.id;meta.maincharListLine list used (1)meta.note;instr.setup;spect.linecharJ/A+A/693/A163/table4bMiscellaneous information on [X/H] determinationrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSpeciesName of speciesphys.atmol.elementcharZAtomic numbermeta.id;meta.mainintListLine list used (1)meta.codecharNline? Number of lines used (2)meta.numberintnullable[X/H]mean? Weighted mean of [X/H] (3)log(Sun)phys.atmol.wOscStrength;stat.meanfloatnullables_[X/H]mean? Weighted standard deviation of [X/H] (3)log(Sun)stat.stdevfloatnullableJ/A+A/693/A163/table5aDerived chemical abundances [X/Fe][Ca/Fe]? [Ca/Fe] abundancelog(Sun)phys.abundfloatnullableListLine list used (1)meta.codecharo_[Ti/Fe]? Number of lines used for [Ti/Fe] (2)meta.numberintnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of RSGmeta.id;meta.mainchar[Na/Fe]? [Na/Fe] abundancelog(Sun)phys.abundfloatnullableb_[Na/Fe]? Lower confidence bound of [Na/Fe]log(Sun)stat.fit.paramfloatnullableB_[Na/Fe]? Upper confidence bound of [Na/Fe]log(Sun)stat.fit.paramfloatnullableo_[Na/Fe]? Number of lines used for [Na/Fe] (2)meta.numberintnullable[Mg/Fe]? [Mg/Fe] abundancelog(Sun)phys.abundfloatnullableb_[Mg/Fe]? Lower confidence bound of [Mg/Fe]log(Sun)stat.fit.paramfloatnullableB_[Mg/Fe]? Upper confidence bound of [Mg/Fe]log(Sun)stat.fit.paramfloatnullableo_[Mg/Fe]? Number of lines used for [Mg/Fe] (2)meta.numberintnullable[Al/Fe]? [Al/Fe] abundancelog(Sun)phys.abundfloatnullableb_[Al/Fe]? Lower confidence bound of [Al/Fe]log(Sun)stat.fit.paramfloatnullableB_[Al/Fe]? Upper confidence bound of [Al/Fe]log(Sun)stat.fit.paramfloatnullableo_[Al/Fe]? Number of lines used for [Al/Fe] (2)meta.numberintnullable[Si/Fe]? [Si/Fe] abundancelog(Sun)phys.abundfloatnullableb_[Si/Fe]? Lower confidence bound of [Si/Fe]log(Sun)stat.fit.paramfloatnullableB_[Si/Fe]? Upper confidence bound of [Si/Fe]log(Sun)stat.fit.paramfloatnullableo_[Si/Fe]? Number of lines used for [Si/Fe] (2)meta.numberintnullable[K/Fe]? [K/Fe] abundancelog(Sun)phys.abundfloatnullableb_[K/Fe]? Lower confidence bound of [K/Fe]log(Sun)stat.fit.paramfloatnullableB_[K/Fe]? Upper confidence bound of [K/Fe]log(Sun)stat.fit.paramfloatnullableo_[K/Fe]? Number of lines used for [K/Fe] (2)meta.numberintnullableb_[Ca/Fe]? Lower confidence bound of [Ca/Fe]log(Sun)stat.fit.paramfloatnullableB_[Ca/Fe]? Upper confidence bound of [Ca/Fe]log(Sun)stat.fit.paramfloatnullableo_[Ca/Fe]? Number of lines used for [Ca/Fe] (2)meta.numberintnullable[Ti/Fe]? [Ti/Fe] abundancelog(Sun)phys.abundfloatnullableb_[Ti/Fe]? Lower confidence bound of [Ti/Fe]log(Sun)stat.fit.paramfloatnullableB_[Ti/Fe]? Upper confidence bound of [Ti/Fe]log(Sun)stat.fit.paramfloatnullable[Cr/Fe]? [Cr/Fe] abundancelog(Sun)phys.abundfloatnullableb_[Cr/Fe]? Lower confidence bound of [Cr/Fe]log(Sun)stat.fit.paramfloatnullableB_[Cr/Fe]? Upper confidence bound of [Cr/Fe]log(Sun)stat.fit.paramfloatnullableo_[Cr/Fe]? Number of lines used for [Cr/Fe] (2)meta.numberintnullable[Ni/Fe]? [Ni/Fe] abundancelog(Sun)phys.abundfloatnullableb_[Ni/Fe]? Lower confidence bound of [Ni/Fe]log(Sun)stat.fit.paramfloatnullableB_[Ni/Fe]? Upper confidence bound of [Ni/Fe]log(Sun)stat.fit.paramfloatnullableo_[Ni/Fe]? Number of lines used for [Ni/Fe] (2)meta.numberintnullable[Y/Fe]? [Y/Fe] abundancelog(Sun)phys.abundfloatnullableb_[Y/Fe]? Lower confidence bound of [Y/Fe]log(Sun)stat.fit.paramfloatnullableB_[Y/Fe]? Upper confidence bound of [Y/Fe]log(Sun)stat.fit.paramfloatnullableo_[Y/Fe]? Number of lines used for [Y/Fe] (2)meta.numberintnullableJ/A+A/693/A163/table5bMiscellaneous information on [X/Fe] determinationrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSpeciesName of speciesphys.atmol.elementcharZAtomic numbermeta.id;meta.mainintListLine list used (1)meta.codecharNline? Number of lines used (2)meta.numberintnullable[X/Fe]mean? Weighted mean of [X/Fe] (3)log(Sun)phys.atmol.wOscStrength;stat.meanfloatnullables_[X/Fe]mean? Weighted standard deviation of [X/Fe] (3)log(Sun)stat.stdevfloatnullableJ/A+A/693/A163/tabled1Line list from VALD3 and MB99recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda(V)? Wavelength in air (VALD3)0.1nmem.wldoublenullableEP(V)? Excitation potential (VALD3)eVphys.atmol.excitationfloatnullableloggf(V)? Oscillator strength (VALD3)phys.atmol.oscStrengthfloatnullablelogtau(V)? Rosseland-mean optical depth of the line-forming layer (VALD3)phys.absorption.opticalDepthfloatnullabledOnlyOne(V)? Depth (VALD3)phot.flux.density;arith.difffloatnullablebeta1(V)? Contamination fraction in line core (VALD3)phys.atmolfloatnullablebeta2(V)? Contamination fraction in line wing (VALD3)phys.atmolfloatnullableNi(V)? Number of stars having valid [X/H] measurements (VALD3)meta.numberintnullableDeltaXH(V)? Correction term to [X/H] measurement (VALD3)phys.atmolfloatnullablelambda(M)? Wavelength in air (MB99)0.1nmem.wldoublenullableEP(M)? Excitation potential (MB99)eVphys.atmol.excitationfloatnullableloggf(M)? Oscillator strength (MB99)phys.atmol.oscStrengthfloatnullablelogtau(M)? Rosseland-mean optical depth of the line-forming layer (MB99)phys.absorption.opticalDepthfloatnullabledOnlyOne(M)? Depth (MB99)phot.flux.density;arith.difffloatnullablebeta1(M)? Contamination fraction in line core (MB99)phys.atmolfloatnullablebeta2(M)? Contamination fraction in line wing (MB99)phys.atmolfloatnullableNi(M)? Number of stars having valid [X/H] measurements (MB99)meta.numberintnullableDeltaXH(M)? Correction term to [X/H] measurement (MB99)phys.atmolfloatnullableSpeciesElement and ionization stagephys.atmol.ionStage;phys.atmol.ionizationcharUsed(V)[YN-] Whether line was used (VALD3)meta.codecharUsed(M)[YN-] Whether line was used (MB99)meta.codechar