Abstract
By using new laboratory data for the carbon spectra C II and, especially, C III, and by paying thorough attention to predicted transitions between high quantum states in C IV, it has been possible to arrive at a practically complete identification of the emission bands recorded in the spectra of Wolf-Rayet stars, including the infra-red region. The dominance of carbon in the WC sequence is confirmed. The identification of a number of essentially unblended, strictly hydrogen-like transitions in C IV, e.g. 6–7, 6–9, 7–10, and 7–12, for which transition probabilities can be exactly calculated, should provide improved posibilities for a study of the excitation mechanism in these stars.
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