High signal4onoise observations of hydrogen- and helium-line profiles in the spectrum of P Cyg show a new feature-broad weak emission wings extending to :1: 1500 km 1 from the line center. The wings are attributed to electron scattering in the extended atmosphere above the line formation region. A simple model calculation shows that an optical depth Te 0.2 for the electron scattering layer will fit the Ha observations. The broad wings are stronger for the He I lines and Te 0.4 is suggested. Key words: broad emission lines-stellar atmospheres-P Cygni stars-electron scattering