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Fig. 3

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Smoothed Hα line-emission components (red profiles). The emission residual intensities are relative to the photospheric line calculated according to the astrophysical parameters (Teff, log g, V sin i) of each object. The figure shows the photospheric component broadened by rotation (blue profiles). It includes the empirical pseudo-photospheric component (green profiles, see Sect. 6.1) in cases of partial emission feeling up of the absorption photospheric line. For the stars 103000272, 110681176, 110747131, and 110827583, the fit of the observed pseudo-photospheric absorption component closely reproduces the actual photospheric line.

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