J/MNRAS/493/2996ivo://CDS.VizieR/J/MNRAS/493/2996doi:10.26093/cds/vizier.74932996CDSMarini E.Dell'Agli F.Di Criscienzo M.Garcia-Hernandez D.A.,Ventura P.Groenewegen M.A.T.Mattsson L.Kamath D.Puccetti S.,Tailo M.Villaver E.2024-08-20T20:16:27Z2023-07-19T14:06:56ZCDS support team

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

cds-question@unistra.frgiant-starslate-type-starsmagellanic-cloudschemically-peculiar-starsinfrared-astronomyWe study the M-type asymptotic giant branch (AGB) population of the Large Magellanic Cloud (LMC) by characterizing the individual sources in terms of the main properties of the progenitors and of the dust present in the circumstellar envelope. To this aim we compare the combination of the spectroscopic and photometric data collected by Spitzer, complemented by additional photometric results available in the literature, with results from AGB modelling that include the description of dust formation in the wind. To allow the interpretation of a paucity stars likely evolving through the post-AGB phase, we extended the available evolutionary sequences to reach the PN phase. The main motivation of the present analysis is to prepare the future observations of the evolved stellar populations of Local Group galaxies that will be done by the James Webb Space Telescope (JWST), by identifying the combination of filters that will maximize the possibilities of characterizing the observed sources. The present results show that for the M-star case the best planes to be used for this purpose are the colour magnitude ([F770W]-[F2550W], [F770W]) and (K_S_-[F770W], [F770W]) planes. In these observational diagrams the sequences of low-mass stars evolving in the AGB phases before the achievement of the C-star stage and of massive AGBs experiencing hot bottom burning are clearly separated and peculiar sources, such as post-AGB, dual-dust chemistry, and iron-dust stars can be easily identified.2020MNRAS.493.2996Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/493/2996CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/609/A114 : Local Group AGB stars and red supergiantsJ/MNRAS/427/3209 : Galactic and MC O-AGBs and RSGs stars (Jones+, 2012)J/MNRAS/440/631 : IR photometry of LMC O-rich evolved stars (Jones+, 2014)J/PASP/122/683 : SAGE-Spec Spitzer legacy program (Kemper+, 2010)J/MNRAS/411/1597 : LMC point source classification in SAGE-Spec (Woods+, 2011)J/AcA/59/239 : VI light curves of LMC long-period variableshttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/493/2996https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/493/2996http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/493/2996https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/493/2996https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/493/2996http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/493/2996GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/493/2996/table2 (The summary of the overall interpretation of the LMC sources analysed in this work, including the interpretation by Groenewegen & Sloan (2018A&A...609A.114G, Cat. J/A+A/609/A114))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/493/2996/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/493/2996/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/493/2996/table2?GETtext/xml+votable180.050000true69.338-70.5790.0055555555555555565/8269 8273-8274 6/33047 33052-33054 33073 33080-33081 33089-33091 33100-33101 33103 33107 33112 33115 33120-33122 33125 33137 37538https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/493/2996?format=asciiInfrareddefaultJ/MNRAS/493/2996/table2The summary of the overall interpretation of the LMC sources analysed in this work, including the interpretation by Groenewegen & Sloan (2018A&A...609A.114G, Cat. J/A+A/609/A114)Fe? Percentage of solid iron derived in this paper%phys.abundintnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSSID[1/4791] Unique spectral identification numbermeta.id;meta.mainintRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainPeriod? OGLE perioddtime.periodintnullableLLuminosity of the source derived in this papersolLumphys.luminosityintSil? Percentage of silicate grains derived in this paper%phys.abundintnullableAl2O3? Percentage of alumina dust derived in this paper%phys.abundintnullabletau10e? Optical depth at 10 micron of the external, oxygen-rich layerphys.absorption.opticalDepthfloatnullableC? Percentage of solid carbon derived in this paper%phys.abundintnullableSiC? Percentage of silicon carbide derived in this paper%phys.abundintnullabletau10i? Optical depth at 10 micron of the internal, carbon-rich layerphys.absorption.opticalDepthfloatnullableTypeEvolutionary characterization determined in this worksrc.classcharLGS18? Luminosity of the source determined in Groenewegen & Sloan (2018A&A...609A.114G, Cat. J/A+A/609/A114)solLumphys.luminosityintnullableSilGS18? Percentage of olivine (MgFeSiO_4_) determined in Groenewegen & Sloan (2018A&A...609A.114G, Cat. J/A+A/609/A114)%phys.abundintnullableAl2O3GS18? Percentage of corundum (Al_2_O_3_) determined in Groenewegen & Sloan (2018A&A...609A.114G, Cat. J/A+A/609/A114)%phys.abundintnullableFeGS18? Percentage of metallic iron determined in Groenewegen & Sloan (2018A&A...609A.114G, Cat. J/A+A/609/A114)%phys.abundintnullable