Evolutionary Stellar Population Synthesis at High Spectral Resolution: Optical Wavelengths

Details Evolutionary Stellar Population Synthesis at High Spectral Resolution: Optical Wavelengths Evolutionary Stellar Population Synthesis at High Spectral Resolution: Optical Wavelengths

2005-01-12

arxiv.org/abs/astro-ph/0501204v1

Mon.Not.Roy.Astron.Soc. 357 (2005) 945-960

Astronomy and Astrophysics

Astrophysics

17 pages, 18 figures, accepted by M.N.R.A.S., results are ready for download from http://www.iaa.csic.es/~rosa (plain ascii ta

Scientific paper

10.1111/j.1365-2966.2005.08692.x

We present the single stellar population (SSP) synthesis results of our new synthetic stellar atmosphere models library with a spectral sampling of 0.3 A, covering the wavelength range from 3000 A to 7000 A for a wide range of metallicities (twice solar, solar, half and 1/10 solar). The stellar library is composed of 1650 spectra computed with the latest improvements in stellar atmospheres. In particular it incorporates non-LTE line-blanketed models for hot (Teff >= 27500 K) and LTE line-blanketed models (Phoenix) for cool (3000 K =< Teff =< 4500 K) stars. Because of the high spectral resolution of this library, evolutionary synthesis models can be used to predict the strength of numerous weak absorption lines, and the evolution of the profiles of the strongest lines over a wide range of ages. The SSP results have been calculated for ages 1 Myr to 17 Gyr using the stellar evolutionary provided by the Geneva and Padova-tracks groups. For young stellar populations, our results have a very detailed coverage of high-temperature stars with similar results for Padova and Geneva isochrones. For intermediate and old stellar populations, our results, once degraded to a lower resolution, are similar to the ones obtained by other groups apart from limitations imposed by the stellar evolutionary physics. The limitations and advantages of our library for the analysis of integrated populations are described. The full set of the stellar library and the evolutionary models are available for retrieval at the websites http://www.iaa.csic.es/~rosa and http://www.iaa.csic.es/~mcs/Sed@, or on request from the first two authors.

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