Rocket-Ultraviolet Spectra of Six Stars in Perseus

Spectra of the 0 and B stars E, , , o, and 40 Per, and liD 24640 have been photographed between 1130 and 2300 A with a pair of rocket-borne ob\ective spectrograpbs. Photospheric lines of He ii, C ii, C iii, C iv, N iii, Ni iv, Si iii, and Si iv and also possibly N V, 0 iv, Al ii, and Al iii have been identified in one or more of the stars. The interstellar La line was measured in , o, and 40 Per, giving an average volume density of 1.7 t 0.5 hydrogen atoms cm -3 in this direction. There appears to be an interstellar contribution to the C ii Al 334.5 line in Per, but otherwise the spectra are too noisy for conclusive detection of the usual ultraviolet interstellar lines of C ii, N I, 0 1, and Sill. The Civ resonance doublet in Per (Bl Ib) has a P Cygni profile with a shift of -900 km s ' in the absorption line, though no such displacement was found in the Si iv pair. For Per (07.5) the resonance lines of N v, Si iv, and C iv all have P Cygni profiles with absorption shifts averaging - 1840 km 5 -`. Smaller velocities were measured for the absorption lines of C iii Al 175.7 and N iv Al 718.5 which arise from excited levels.