Daytime airglow spectra between 530 and 930 ¿ were obtained at ~4 ¿ resolution from a rocket launch at White Sands, New Mexico, June 27, 1980. Portions of the spectrum were observed in second order at ~2¿ resolution. The higher resolution of the present data confirms our previous identification of O II transitions and resolves the identification of O II emission at 537-539 ¿ as due to both a doublet and a quartet component. For the case of viewing at 90¿ to the zenith between 196 and 242 km ~1/3 of the 537-539 ¿ emission originates from the O II 2s2p42P state. We infer a 538/581 ¿ branching ratio of ~3 in agreement with laboratory and calculated values of 1.6 to 3.3. Other O II branching ratios are in agreement with laboratory data. A somewhat low value for the 718/796 ratio in the flight data is interpreted as due to blended N2 emission at 796 ¿. The observed emission rate from the 2s2p42P state is more adequately modeled using partial photoionization cross sections calculated using the dipole velocity rather than the dipole length approximation. This fact must be considered when computing the 834 ¿ emission rate from direct photoionization. N II is seen to be a very minor source of emission below 916 ¿ in the dayglow. The identification ofO II 581 ¿ emission confirms a prediction mde in 1977 by Delaboudini¿re. The O II emission at 581 A;O complicates interpretation of low resolution spectral observations near 584 ¿ in the airglow and also for case of comets and planets where O atoms and O bearing molecules are present.