The ultraviolet spectrum of stars having optical Fe II emission lines.

Analysis of data concerning the fluxes of FeII lines in the optical and the UV for luminous P Cyg stars, symbiotic objects, and Seyfert galaxies is discussed. When fluxes of individual lines are available, semi-empirical methods of deriving information, taking account of self absorption, are most appropriate, and can be interpreted if, for instance, the lines are thought to be formed in a stellar wind. When low resolution data only are available in the UV, methods of spectral synthesis are necessary. Work taking account of emission and absorption lines is described.