First detection of hydroxyl in the atmosphere of Venus

Context. Airglow emissions, such as previously observed from NO and O (0-0) on Venus, provide insight into the chemical and dynamical processes that control the composition and energy balance in the upper atmospheres of planets. The OH airglow emission has been observed previously only in the Earth's atmosphere where it has been used to infer atomic oxygen abundances. The O (0-1) airglow emission also has only been observed in the Earth's atmosphere, and neither laboratory nor theoretical studies have reached a consensus on its transition probability. Aims. We report measurements of night-side airglow emission in the atmosphere of Venus in the OH (2-0), OH (1-0), O (0-1), and O (0-0) bands. This is the first detection of the first three of these airglow emissions on another planet. These observations provide the most direct observational constraints to date on H, OH, and O, key species in the chemistry of Venus' upper atmosphere. Methods. Airglow emission detected at wavelengths of 1.40-1.49 and 2.6-3.14 m in limb observations by the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) on the Venus Express spacecraft is attributed to the OH (2-0) and (1-0) transitions, respectively, and compared to calculations from a photochemical model. Simultaneous limb observations of airglow emission in the O (0-0) and (0-1) bands at 1.27 and 1.58 m, respectively, were used to derive the ratio of the transition probabilities for these bands. Results. The integrated emission rates for the OH (2-0) and (1-0) bands were measured to be and kR respectively, both peaking at an altitude of km near midnight local time for the considered orbit. The measured ratio of the O (0-0) and (0-1) bands is . Conclusions. Photochemical model calculations suggest the observed OH emission is produced primarily via the Bates-Nicolet mechanism, as on the Earth. The observed ratio of the intensities of the O (0-0) and (0-1) bands implies the ratio of their transition probabilities is .