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Fig. B.3


Same as Fig. B.1, but for the He-strong star NGC 3293-034. The grey-shaded boxes guide the eye to recognise the signatures of the chemical peculiarity of the star, i.e., the unusually strong He i lines. Similar to the models employed by Hunter et al. (2009), the present computations with Ads do not account for the pronounced helium enrichment and therefore the altered atmospheric structure of the star. As a consequence, the analysis yields incorrect atmospheric parameters and abundances, despite the fact that a good fit to the hydrogen and many metal lines is achieved.

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