During 1949 and 1950 the spectrum of XX Ophiuchi, then in the bright-line state, was photographed from x 3600 to H with a dispersion of 10 A/mm; from H to Ha with 15 A/mm. Of the emission lines listed in Table 2, 29 are of II, 14 of He I, 72 of neutral metals, 441 of ionized metals, 11 miscellaneous, and 10 unidentified. The total number, 577, is possibly the greatest yet measured in any stellar spectrum. Lines of Fe ii dominate the spectrum; certain multiplets are observed more completely than in the laboratory. The D lines of sodium are conspicuous in emission-a rare occurrence in stellar spectra. The velocities from the bright lines have not changed markedly since 1921; in 1949 weak absorption components on the shortward edges of bright metallic lines had but a slight effect. H and [0 2] lines yield the same velocities as metarnc lines. In 1949 the H and K lines of Ca ii had well-defined, greatly displaced absorption components something like those in the spectrum of HD 190073. In XX Ophiuchi these lines are subject to large variations. The bright metallic lines are stronger than in other 3e stars exhibiting the same range of atomic excitation. This indicates a larger emitting atmosphere.