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Fig. B.2

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Same as Fig. B.1, but for the star NGC 2004-053. This is an example for a model fit to a Be star seen pole-on. The grey-shaded box guides the eye to recognise the signature of the presence of a disc, i.e., the Hα emission. Similar to the models employed by Hunter et al. (2009), the present computations with Ads do not account for the presence of a disc and gravity darkening. The neglect of the true nature of this star yields potentially biased atmospheric parameters and abundances, despite the fact that a good fit to many spectral lines is achieved.

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