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Fig. 1.


Number density of H vs. optical depth log τRoss for three different abundances of Mg. The blue line (A(Mg) = 7.58) corresponds to the solar abundance of Mg, the red line to the Mg abundance in Pisces II 10694, and the black line (A(Mg) = 5.54) to the Mg abundance expected for a normal metal-poor star with [Fe/H] = −2.6. The molecular bands and the metallic lines are mainly formed between log τRoss = −2 and −1, a region where the number density of H is strongly affected by the Mg abundance.

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