Free Access
Volume 542, June 2012
Article Number A104
Number of page(s) 7
Section Stellar atmospheres
Published online 15 June 2012

Online material

thumbnail Fig. 2

Relative-to-solar iron abundance from derived Fe i lines versus excitation potential for Arcturus and for SRd stars of our program. As is the convention in spectroscopic literature, hereafter we denote the relative-to-solar abundance of a certain element as [El/H] = log ϵ(El) – log ϵ(El).

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thumbnail Fig. 3

Relative-to-solar iron abundances derived from the Fe i lines versus the equivalent widths of Arcturus and SRd stars in our program.

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© ESO, 2012

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