George Wallerstein, Thomas Gomez, Wenjin Huang
The GAIA satellite is likely to observe thousands of RR Lyrae stars within a
small spectral window, between 8470A and 8750A, at a resolution of 11,500. In
order to derive the metallicity of RR Lyrae stars from Gaia, we have obtained
numerous spectra of RR Lyrae stars at a resolution of 35,000 with the Apache
Point Observatory 3.5 m echelle spectrograph. We have correlated the Ca II
triplet line strengths with metallicity as derived from Fe II abundances,
analogous to Preston's (1959) use of the Ca II K line to estimate the
metallicity of RR Lyrae stars. The Ca II line at 8498A is the least blended
with neighboring Paschen lines and thus provides the best correlation.
View original:
http://arxiv.org/abs/1108.4986
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