New Grids of Synthetic Spectra for Abundance Derivation and Population Synthesis

Details New Grids of Synthetic Spectra for Abundance Derivation and Population Synthesis New Grids of Synthetic Spectra for Abundance Derivation and Population Synthesis

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999iaus..192..365b&link_type=abstract

The stellar content of Local Group galaxies, Proceedings of the 192nd symposium of the International Astronomical Union held in

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We have built a new grid of synthetic spectra in the wavelength range lambdalambda 4600-5600 Angstroms for [alpha-elements/Fe] = 0.0 and +0.4. This grid is used in combination with an observed spectra library of reference stars in order to derive stellar parameters from low to medium resolution spectra of faint stars. The basis of the method was described in Cayrel et al. (1991, A&A 247, 108) and Meliani et al. (1995, A&A, 300, 349). For the calculation of this new grid already available, the set of atomic and molecular constants were revised and model atmospheres with overshooting parameter appropriate to reproduce the Hβ line wings (suitable to indicate temperatures) were employed. The method is applied to Galactic halo faint stars, bulge stars and Magellanic Cloud stars. It would be suitable also to analyse stars in other nearby galaxies. A computation of a high-resolution grid of spectra in the range lambdalambda 3800-7000 Angstroms, to be used in the context of echelle spectrographs (and also at low resolution), as well as a full grid in the range lambdalambda 3800-10200 Angstroms, to be further used in conjunction with evolutionary population synthesis models are also underway.

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