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Fig. 1

image

Synthesis of the Zr ii line at 4208 Å in the solar spectrum (in this case Vesta, observed with the MIKE spectrograph in January 2006). The upper panel shows synthetic spectra with different Zr abundances in steps of 0.04 dex (blue lines). The difference between the observed spectrum and the synthetic spectra is plotted in the lower panel with the best abundance spectrum plotted as a red line in both the upper and lower panels. The inset shows the χ2 fit to determine the best abundance value expressed as log ϵ(Zr) (shown as a red dot).

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