J/A+AS/130/513ivo://CDS.VizieR/J/A+AS/130/513CDSGarcia-Vargas M.L.Molla M.Bressan A.1999-03-02T04:31:20Z1999-03-02T05:30:40ZCDS support team

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

cds-question@unistra.frline-intensitiesstellar-evolutionary-modelsWe present theoretical equivalent widths for the sum of the two strongest lines of the calcium triplet, CaT index, in the near-IR ({lambda}{lambda} 8542, 8662{AA}), using evolutionary synthesis techniques and the most recent models and observational data for this feature in individual stars. We compute the CaT index for Single Stellar Populations (instantaneous burst, standard Salpeter-type IMF at four different metallicities, Z=0.004, 0.008, 0.02 (solar) and 0.05, and ranging in age from very young bursts of star formation (few Myr) to old stellar populations, up to 17Gyr, representative of galactic globular clusters, elliptical galaxies and bulges of spirals. The interpretation of the observed equivalent widths of CaT in different stellar systems is discussed. Composite-population models are also computed as a tool to interpret the CaT detections in star-forming regions, in order to disentangle between the component due to Red Supergiant stars, RSG, and the underlying, older, population. CaT is found to be an excellent metallicity-indicator for populations older than 1 Gyr, practically independent of the age. We discuss its application to remove the age-metallicity degeneracy, characteristic of all studies of galaxy evolution based on the usual integrated indices (both broad band colors and narrow band indices). The application of the models computed here to the analysis of a sample of elliptical galaxies will be discussed in a forthcoming paper Gorgas et al. 1997).1998A&AS..130..513Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+AS/130/513CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+AS/130/513https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+AS/130/513http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+AS/130/513https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+AS/130/513https://vizier.iucaa.in/viz-bin/votable?-source=J/A+AS/130/513http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+AS/130/513GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+AS/130/513/table12*Synthetic LuminositiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogAgeCluster agelog(yr)time.agefloatZMetalicity value value relative to the SunSunphys.abund.ZfloatLUVLuminosity in the UV (at 2000{AA})solLumphys.luminosity;em.UVdoubleLoptLuminosity in the optical (at 4850{AA}), representative of the continuum near H{beta}solLumphys.luminositydoubleLIRLuminosity in the infrared (at 2.17{mu}m, near Br_{gamma}_)solLumphys.luminosity;em.IRdoubleJ/A+AS/130/513/table34*Synthetic Calcium Triplet Equivalent Widths, according to Jorgensen et al. (1992A&A...254..258J) theoretical calibrations (II).recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogAgeSingle Stellar Population (SSP) agelog(yr)time.agefloatZMetallicity value relative to the SunSunphys.abund.ZfloatLcontContinuum luminosity from the SSP (1)solLumphys.luminositydoubleLCaIILuminosity absorbed in the Ca II lines at 8542 and 8662{AA} by the stars of the SSPsolLumphys.luminositydoubleEW(CaT)Equivalent width of CaT (2)0.1nmspect.line.eqWidthfloatJ/A+AS/130/513/table56Synthetic Calcium Triplet Equivalent Widths, according to Diaz et al. (1989MNRAS.239..325D, DTT89) empirical calibrations (I).recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogAgeSingle Stellar Population (SSP) agelog(yr)time.agefloatZMetallicity value relative to the SunSunphys.abund.ZfloatLcontContinuum luminosity from the SSP (1)solLumphys.luminositydoubleLCaIILuminosity absorbed in the Ca II lines at 8542 and 8662{AA} by the stars of the SSPsolLumphys.luminositydoubleEW(CaT)Equivalent width of CaT (2)0.1nmspect.line.eqWidthfloatJ/A+AS/130/513/table7Two-Populations composite models according to Jorgensen et al. (1992A&A...254..258J) calibrations.recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintProp? Proportion of the populations considered (1)stat.paramfloatnullableAge1Age of the first population (2)Myrtime.agefloatn_Age1[+] + when more than one populationmeta.notecharAge2? Age of the second populationMyrtime.ageintnullablen_Age2[+] + when more than two populationsmeta.notecharAge3? Age of the third populationMyrtime.ageintnullableZMetallicity value relative to the SunSunphys.abund.ZfloatEW(CaT)Equivalent width of CaT in absorption0.1nmspect.line.eqWidthfloatEW(Hb)? Equivalent width of H{beta} in emission (3)0.1nmspect.line.eqWidthfloatnullableJ/A+AS/130/513/table8Three-Populations composite models according to Jorgensen et al. (1992A&A...254..258J) calibrations.recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintProp? Proportion of the populations considered (1)stat.paramfloatnullableAge1Age of the first population (2)Myrtime.agefloatn_Age1[+] + when more than one populationmeta.notecharAge2? Age of the second populationMyrtime.ageintnullablen_Age2[+] + when more than two populationsmeta.notecharAge3? Age of the third populationMyrtime.ageintnullableZMetallicity value relative to the SunSunphys.abund.ZfloatEW(CaT)Equivalent width of CaT in absorption0.1nmspect.line.eqWidthfloatEW(Hb)? Equivalent width of H{beta} in emission (3)0.1nmspect.line.eqWidthfloatnullableJ/A+AS/130/513/table9Two-Populations composite models according to Diaz et al. (1989MNRAS.239..325D) calibrations.recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintProp? Proportion of the populations considered (1)stat.paramfloatnullableAge1Age of the first population (2)Myrtime.agefloatn_Age1[+] + when more than one populationmeta.notecharAge2? Age of the second populationMyrtime.ageintnullablen_Age2[+] + when more than two populationsmeta.notecharAge3? Age of the third populationMyrtime.ageintnullableZMetallicity value relative to the SunSunphys.abund.ZfloatEW(CaT)Equivalent width of CaT in absorption0.1nmspect.line.eqWidthfloatEW(Hb)? Equivalent width of H{beta} in emission (3)0.1nmspect.line.eqWidthfloatnullableJ/A+AS/130/513/table10Three-Populations composite models according to Diaz et al. (1989MNRAS.239..325D) calibrations.recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintProp? Proportion of the populations considered (1)stat.paramfloatnullableAge1Age of the first population (2)Myrtime.agefloatn_Age1[+] + when more than one populationmeta.notecharAge2? Age of the second populationMyrtime.ageintnullablen_Age2[+] + when more than two populationsmeta.notecharAge3? Age of the third populationMyrtime.ageintnullableZMetallicity value relative to the SunSunphys.abund.ZfloatEW(CaT)Equivalent width of CaT in absorption0.1nmspect.line.eqWidthfloatEW(Hb)? Equivalent width of H{beta} in emission (3)0.1nmspect.line.eqWidthfloatnullable