Observations of Jupiter’s Hydrogen Airglow by Juno-UVS

While the primary function of the Juno spacecraft’s Ultraviolet Spectrograph (UVS) during perijoves is to observe Jupiter’s auroral features, it is also capable of detecting and measuring Jupiter’s airglow. Jupiter’s airglow is caused, in part, by hydrogen emission signatures. The UV photons are emitted after photoionized gas in Jupiter’s upper atmosphere returns to its ground state. Juno’s low altitude perijove allows for UVS to detect Hydrogen Lyman-alpha emissions as a function of zenith angle. We search for variation in this emission, based on a variety of criteria, including spacecraft latitude, longitude, local time information, solar zenith angle, and location with respect to certain features (e.g., the "Great Blue Spot" magnetic anomaly, the magnetic equator). We will describe attempts to detect and characterize spectrally these emissions with Juno-UVS.