High resolution far ultraviolet (12W2000,4) spectra of 17 cool giant and supergiant stars have been obtained using the IUE satellite of ESA, NASA and UK. We have measured the line intensities, wavelengths and widths of approximately 200 EUV emission lines in these spectra, using a least squares gaussian fitting technique. Line identification has been obtained in about one third of the cases. The measured values are organized in a database in order to facilitate updating and investigation of interrelations with stellar atmospheric parameters.The observations include lines from C I. C 11, C IV, S I, 0 I, 0 IV, Si 11, Si IV, N V, A1 111. Fe I1 and Mg 11. These lines are mostly formed by radiative processes in the extremely rarefied plasma in the outer stellar atmospheres, and occasionally involve highly excited energy levels of the atoms and ions. The temperature of formation ranges from about 5 x lo' to IO5 K, corresponding to different depth levels in the atmosphere, and the lines serve as a valuable tool for probing the physical conditions in these regions. We may also get new information on atomic processes that take place under conditions that are never duplicated in the laboratory. The present data may therefore give important contributions both to astrophysics and to atomic physics.