J/AJ/157/167ivo://CDS.VizieR/J/AJ/157/167doi:10.26093/cds/vizier.51570167CDSDicenzo B.Levesque E.M.2019-11-13T14:20:37Z2019-08-06T07:22:58ZCDS support team

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

cds-question@unistra.frmilky-way-galaxymagellanic-cloudslate-type-starssupergiant-starsstellar-spectral-typeseffective-temperatureline-intensitiesRed supergiants (RSGs) are evolved massive stars that represent extremes, in both their physical sizes and their cool temperatures, of the massive star population. The effective temperature (T_eff_) is the most critical physical property needed to place an RSG on the Hertzsprung-Russell Diagram, due to the stars' cool temperatures and resulting large bolometric corrections. Several recent papers have examined the potential utility of atomic line equivalent widths (EWs) in cool supergiant (CSG) spectra for determining T_eff_ and other physical properties and found strong correlations between Ti I and Fe I spectral features and T_eff_ in earlier-type CSGs (G and early K) but poor correlations in M-type stars, a spectral subtype that makes up a significant fraction of RSGs. We have extended this work by measuring the EWs of Ti, Fe, and Ca lines in late K- and M-type RSGs in the Milky Way, Large Magellanic Cloud, and Small Magellanic Cloud, and compared these results to the predictions of the theoretical stellar LTE atmosphere models (MARCS) stellar atmosphere models. Our analyses show a poor correlation between T_eff_ and the Fe I and Ti I lines in our observations (at odds with strong correlations predicted by stellar atmosphere models), but do find statistically significant correlations between T_eff_ and the Ca II triplet (CaT) features of Milky Way RSGs, suggesting that this could be a potential diagnostic tool for determining T_eff_ in M-type supergiants. We also examine correlations between these spectral features and other physical properties of RSGs (including metallicity, surface gravity, and bolometric magnitude), and consider the underlying physics driving the evolution of atomic line spectra in RSGs.2019AJ....157..167Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/157/167CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/AJ/126/2867 : Red supergiants in Magellanic Clouds (Massey+, 2003)J/ApJ/749/177 : Yellow and red supergiants in the LMC (Neugent+, 2012)J/ApJ/751/156 : Ti and Fe lines in red supergiants (Bergemann+, 2012)J/ApJ/754/35 : Red supergiant stars in the SMC. II. (Yang+, 2012)J/MNRAS/427/3209 : Galactic and MC O-AGBs and RSGs stars (Jones+, 2012)J/ApJ/822/L5 : Observed red supergiants in the inner GalaxyJ/A+A/616/A175 : Red supergiant stars in the LMC. II. (Yang+, 2018)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/157/167https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/157/167http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/157/167https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/157/167https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/157/167http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/157/167GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/157/167/table1 (stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/157/167/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/157/167/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/157/167/table1?GETtext/xml+votable180.050000true5.351188359.95310250.0055555555555555566/1443 1447 2940 3043 3256 3257 3272 3275 3469 3608 3609 3621 3622 3632 6897 14295 14302 14319 23983 24164 24336 24486 24497 30631 33054 33076 33077 33094 33097 33098 33100 33101 33112 33115 33295 33298 33304 33306 33316 33317 33328https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/157/167?format=asciidefaultJ/AJ/157/167/table1starsSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGalGalaxy namemeta.id.parentcharStarStar namemeta.id;meta.maincharprimaryEWsindicates equivalent widths in Tables 3-5meta.ref.urlcharSpTypeSpectral typesrc.spTypecharTeff[3425/3900] Effective temperatureKphys.temperature.effectiveintb_logg[-0.7/0.6]? Surface gravity, lower valuelog(cm.s**-2)phys.gravity;stat.minfloatnullableB_logg[-0.4]? Surface gravity, upper valuelog(cm.s**-2)phys.gravity;stat.maxfloatnullableb_Mbol[-9.64/-5.77]? Bolometric luminosity, lower valuemagphys.luminosity;stat.minfloatnullableB_Mbol[-8.57]? Bolometric luminosity, upper valuemagphys.luminosity;stat.maxfloatnullableAssocName of OB association(s)meta.id.parentchar_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/AJ/157/167/EWsCa I, CaT (table 3) , Fe I (table 4) and Ti I (table 5) equivalent widthsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGalGalaxy namemeta.id.parentcharStarStar namemeta.id;meta.maincharEW(6572)[0.285/0.43] Equivalent width of Ca I 6572{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8498)[1.44/2.85] Equivalent width of Ca II 8498{AA} ({AA})0.1nmspect.line.eqWidthfloatEW(8542)[1.76/5.29] Equivalent width of Ca II 8542{AA} ({AA})0.1nmspect.line.eqWidthfloatEW(8662)[2.34/4.5] Equivalent width of Ca II 8662{AA} ({AA})0.1nmspect.line.eqWidthfloatEW(8514.1)[0.19/1.103] Equivalent width of Fe I 8514.1{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8582.0)[0.094/0.455] Equivalent width of Fe I 8582.0{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8611.0)[0.069/0.501] Equivalent width of Fe I 8611.0{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8679.4)[0.021/0.087] Equivalent width of Fe I 8679.4{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8688.5)[0.361/1.205] Equivalent width of Fe I 8688.5{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8710.2)[0.012/0.283] Equivalent width of Fe I 8710.2{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8712.8)[0.091/0.546] Equivalent width of Fe I 8712.8{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8757.0)[0.222/0.609] Equivalent width of Fe I 8757.0{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8793.2)[0.162/0.475] Equivalent width of Fe I 8793.2{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8805.0)[0.212/0.803] Equivalent width of Fe I 8805.0{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8824.0)[0.342/1.438] Equivalent width of Fe I 8824.0{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8838.0)[0.03/1.031] Equivalent width of Fe I 8838.0{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8518.1)[0.055/0.543] Equivalent width of Ti I 8518.1{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8683.0)[0.201/0.701] Equivalent width of Ti I 8683.0{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8692.0)[0.168/0.463] Equivalent width of Ti I 8692.0{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8730.5)[0.011/0.212] Equivalent width of Ti I 8730.5{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.IfloatEW(8734.5)[0.055/0.362] Equivalent width of Ti I 8734.5{AA} ({AA})0.1nmspect.line.eqWidth;em.opt.Ifloat