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Effects of Non-Solar Abundance Ratios on Star Spectra: Observations versus Models

Published online by Cambridge University Press:  17 August 2012

Anne E. Sansom ,
André de Castro Milone ,
Alexandre Vazdekis  and
Patricia Sánchez-Blázquez
Anne E. Sansom
Affiliation:
Jeremiah Horrocks Institute, University of Central Lancashire, Preston, Lancs PR1 2HE, UK email: [email protected]
André de Castro Milone
Affiliation:
Divisão de Astrofísica, Instituto Nacional de Pesquisas Espaciais, Av. dos Astronautas 1758, São José dos Campos, SP 12227-010, Brazil
Alexandre Vazdekis
Affiliation:
Instituto de Astrofísica de Canarias, La Laguna, E-38200 Tenerife, Spain
Patricia Sánchez-Blázquez
Affiliation:
Departamento de Física Teórica, Universidad Autónoma de Madrid, 28409, Spain
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Abstract

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Element abundance ratios hold important clues to understanding the evolution of stellar populations, through the varying timescales of different nucleosynthetic contributors. Newly measured and compiled [Mg/Fe] ratios in the MILES stellar library are used to confront models of star spectra. Such models have been used in recent years to provide estimates of differential changes in spectral line strengths, due to enhancements in [α/Fe]. In this paper we test one widely used set of theoretical element response functions. Using magnesium as a proxy for all alpha elements we test the reliability of these theoretical response functions against empirical observations, and thus the reliability of current methods of measuring element abundance ratios in the stellar populations.

Keywords

stars: atmospheresstars: abundancestechniques: spectroscopic
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S284: The Spectral Energy Distribution of Galaxies , September 2011 , pp. 12 - 15
Copyright
Copyright © International Astronomical Union 2012

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