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Fig. 1

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Top: comparison of our high-resolution morphological spectral types and those attributed by Walborn by means of low-resolution photographic spectra (Δλ = 1.2 Å), for 14 stars (dwarfs and giants) in common. The X-scale corresponds to spectral types from O2 to B2. Stars considered/suspected to be SBs are additionally marked with large circles. Bottom: the spectral type discrepancy as a function of vsini . To eliminate binarity effects on the observed vsini , stars considered/suspected to be SBs have been discarded. Note that the adopted vsini -estimates do not account for the effects of macroturbulence.

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