J/A+A/503/913ivo://CDS.VizieR/J/A+A/503/913doi:10.26093/cds/vizier.35030913CDSAringer B.Girardi L.Nowotny W.Marigo P.Lederer M.T.2014-12-08T10:06:02Z2009-10-29T22:17:43ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelsphotometryspectroscopyCarbon rich objects represent an important phase during the late stages of evolution of low and intermediate mass stars. They contribute significantly to the chemical enrichment and to the infrared light of galaxies. A proper description of their atmospheres is crucial for the determination of fundamental parameters such as effective temperature or mass loss rate. We study the spectroscopic and photometric properties of carbon stars. In the first paper of this series we focus on objects that can be described by hydrostatic models neglecting dynamical phenomena like pulsation and mass loss. As a consequence, the reddening due to circumstellar dust is not included. Our results are collected in a database, which can be used in conjunction with stellar evolution and population synthesis calculations involving the AGB. We have computed a grid of 746 spherically symmetric COMARCS atmospheres covering effective temperatures between 2400 and 4000K, surface gravities from log(g[cm/s^2^])=0.0 to -1.0, metallicities ranging from the solar value down to one tenth of it and C/O ratios in the interval between 1.05 and 5.0. Subsequently, we used these models to create synthetic low resolution spectra and photometric data for a large number of filter systems. The tables including the results are electronically available. First tests of the application on stellar evolution calculations are shown. We have selected some of the most commonly used colours in order to discuss their behaviour as a function of the stellar parameters. A comparison with measured data shows that down to 2800K the agreement between predictions and observations of carbon stars is good and our results may be used to determine quantities like the effective temperature. Below this limit the synthetic colours are much too blue. The obvious reason for these problems is the neglect of circumstellar reddening and structural changes due to pulsation and mass loss.2009A&A...503..913Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/503/913CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/503/913https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/503/913http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/503/913https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/503/913https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/503/913http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/503/913GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/503/913/spectraList of spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMod[1/746] Model numbermeta.id;meta.mainintVer[3/4] Version of COMARCS modelmeta.softwareintTeff[2400/4000] Effective temperatureKphys.temperature.effectiveintlogg[-1.00/+0.00] Surface gravitylog(cm.s**-2)phys.gravityfloatMass[1/99] MasssolMassphys.massfloatZ(0.10, 0.33, 1.00) Metallicity (in solar metallicity)Sunphys.abund.ZfloatC/O[1.05/5.00] C/O abundance ratiophys.abund;arith.ratiofloatxi[2.5] Microturbulent velocitykm/sphys.velocfloatSpFileNameName of the spectrum in subdirectory specmeta.id;meta.filecharSpPlot of the spectrummeta.ref.urlcharJ/A+A/503/913/photomList of photometric system filesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFileNameName of the file in subdirectory photmeta.id;meta.filecharFiltFilters for which bolometric corrections are presented in the filemeta.code;instr.filterchar