Emission lines in 32 Cygni

With the exception of a very few weak lines, all of these are also seen in zeta Aur during its eclipse, and the stronger features appear in 31 Cyg. Seventy-four percent of these emission lines can be attributed to FeII.

Few are intrisically weaker than gf~0.01. Other spectra definitely present are CII, NI, OI, SiII, MgII, SII, CrII, NiII, AlII, AlIII, FIII, SiIV, and CIV. No emission lines of the neutral metals, except for fluorescent FeI UV44, are unambiguously detected; specifically, lines of CI, SiI, or SI were not detected in the spectrum.