Bibcode
Sánchez-Blázquez, P.; Vazdekis, A.; de Castro Milone, A. ; Sansom, A. E.
Referencia bibliográfica
Monthly Notices of the Royal Astronomical Society, Volume 435, Issue 2, p.952-974
Advertised on:
10
2013
Número de citas
25
Número de citas referidas
19
Descripción
A method that is widely used to analyse stellar populations in galaxies
is to apply the theoretically derived responses of stellar spectra and
line indices to element abundance variations, which are hereafter
referred to as response functions. These are applied in a differential
way, to base models, in order to generate spectra or indices with
different abundance patterns. In this paper, sets of such response
functions for three different stellar evolutionary stages are tested
with new empirical [Mg/Fe] abundance data for the medium-resolution
Isaac Newton Telescope library of empirical spectra (MILES). Recent
theoretical models and observations are used to investigate the effects
of [Fe/H], [Mg/H] and overall [Z/H] on spectra, via ratios of spectra
for similar stars. The global effects of changes in abundance patterns
are investigated empirically through direct comparisons of similar stars
from MILES, highlighting the impact of abundance effects in the blue
part of the spectrum, particularly for lower temperature stars. It is
found that the relative behaviour of iron-sensitive line indices are
generally well predicted by response functions, whereas Balmer line
indices are not. Other indices tend to show large scatter about the
predicted mean relations. Implications for element abundance and age
studies in stellar populations are discussed and ways forward are
suggested to improve the match with the behaviour of spectra and
line-strength indices observed in real stars.
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