The methods of determining [Fe/H] for RR Lyrae stars

Details The methods of determining [Fe/H] for RR Lyrae stars The methods of determining [Fe/H] for RR Lyrae stars

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006pabei..24..308w&link_type=abstract

Progress in Astronomy (ISSN 1000-8349), Vol. 24, No. 4, p. 308 - 318 (2006)

Astronomy and Astrophysics

Astrophysics

Astrophysics, Rr Lyrae Stars, Review, Galaxy Structure, Abundances

Scientific paper

The fact that the absolute light of RR Lyrae stars is affected by its metal abundance requires us to determine its metal abundance when it is used as accurate indicator for distance. While in principle the most fundamental way to determine the abundance of RR Lyrae stars is via high dispersion spectroscopy, in practice this method is limited to the brightest stars in the nearest distance to the Sun. This restriction has led over the years to the development of a large number of techniques that measure in various ways such as ΔS method, Caby photometry and Fourier parameters of light curves. This paper primarily reviews these three methods. The ΔS method is using the ΔS metallicity index which is calculated from equivalent width of lines Hδ, Hγ, Hβ and Ca II K in low resolution spectrum to determine the abundance of RR Lyrae stars. The photometric method, Caby, employs the correlation between hk index and metal abundance to calculate metal abundance for RR Lyrae stars. The method of Fourier parameters is using the experimental relation between the parameters of light curve of RR Lyrae star and metal abundance to determine its metallicity. Although these three methods are all using the experimental relation between their spectral indices and metal abundance, they have different accuracy and condition for usage. The detailed discussion and comparison on these methods are also given in this paper to provide reference for the observer to make a choice based on their advantages and disadvantages.

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