Chemical abundances of fast-rotating massive stars - I. Description of the methods and individual results

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Fig. E.4

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Same as Fig. E.1, but for HD 14442 (O5n(f)p; vsin i = 285 km s^-1). Because wind parameters were not derived, wind-sensitive lines are not well reproduced: too much emission is seen in He ii 4686 for the best-fit model, but too little emission for the neighbouring N iii 4634–4643 lines.

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