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Evolutionary stellar population synthesis at high spectral resolution: optical wavelengths

Delgado, R. M. González ; Cerviño, M. ; Martins, L. P. ; Leitherer, C. ; Hauschildt, P. H.

Monthly notices of the Royal Astronomical Society, 2005-03, Vol.357 (3), p.945-960 [Periódico revisado por pares]

Oxford, UK: Blackwell Science Ltd

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  • Título:
    Evolutionary stellar population synthesis at high spectral resolution: optical wavelengths
  • Autor: Delgado, R. M. González ; Cerviño, M. ; Martins, L. P. ; Leitherer, C. ; Hauschildt, P. H.
  • Assuntos: galaxies: evolution ; galaxies: stellar content ; stars: evolution
  • É parte de: Monthly notices of the Royal Astronomical Society, 2005-03, Vol.357 (3), p.945-960
  • Notas: istex:94857096E3ED678B4BC1A1EEE4428F4FFAD27760
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    ObjectType-Article-2
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  • Descrição: We present the single stellar population (SSP) synthesis Results of our new synthetic stellar atmosphere models library with a spectral sampling of 0.3 Å, covering the wavelength range from 3000 to 7000 Å for a wide range of metallicities (twice solar, solar, half solar 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-local thermodynamic equilibrium (LTE) line-blanketed models for hot (Teff≥ 27 500 K), and LTE line-blanketed models (Phoenix) for cool (3000 ≤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 from 1 Myr to 17 Gyr using the stellar evolutionary tracks provided by the Geneva and Padova groups. For young stellar populations, our Results have a very detailed coverage of high-temperature stars with similar Results for the 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 (limitations imposed by the stellar evolutionary physics notwidthstanding). The limitations and advantages of our models 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/~/sed@, or on request from the first two authors.
  • Editor: Oxford, UK: Blackwell Science Ltd
  • Idioma: Inglês
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  • Realização: ABCD-USP USP   Logos de Redes Sociais: Freepik

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