Fig. 2
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Sequence of late O supergiant (Sk −71∘ 41, 09.5 Ib, this study), late O hypergiant (Sk −69∘ 279, ON9.5 Ia+, this study) and very late WN star (Sk −67∘ 266, WN11h, Crowther & Smith 1997) in the LMC, illustrating the transition from absorption line dominated stars to emission line dominated (e.g. He I λ4471, He II λ4686). Note that Balmer lines include nebular contributions for Sk −67∘ 266 (S61).
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