Spatial variability of CH4 and C2H2 absorptions in Jupiter's auroral regions from Juno-UVS observations

Color ratios derived from molecular hydrogen emissions provide valuable diagnostics for the energy of precipitating electrons and the structure of the auroral atmosphere. We aim to characterize the horizontal and vertical variability of hydrocarbon absorption in Jupiter's auroral atmosphere using ultraviolet data from the Juno-UVS spectrograph and to investigate potential departures from the expected structure. We constructed color ratio maps sensitive to CH$_4$ and C$_2$H$_2$ absorptions for perijoves (PJs) 6 and 10, two of Juno's close approaches to Jupiter, by integrating auroral H$_2$ emission over hydrocarbon-sensitive spectral intervals. For CH$_4$, we redefined the absorbed spectral band, replacing the traditionally used 125-130 nm interval with 135-140 nm, in order to mitigate higher-order calibration issues. In regions of intense auroral brightness, we developed a correction method to account for spectral distortion due to detector non-linearities at high fluxes. CH$_4$ and C$_2$H$_2$ absorptions generally follow the expected vertical distribution, with the CH$_4$ density extending to higher altitudes than C$_2$H$_2$. However, several localized regions show unexpected spatial distribution of the absorption. In PJ6, such anomalies are attributed to instrumental non-linearities. After correction, the CR distributions become consistent with standard hydrocarbon vertical distributions. In PJ10, however, some anomalous patterns persist despite correction. Spectral modeling indicates that these can be explained by modifying the relative abundances of CH$_4$ and C$_2$H$_2$, suggesting horizontal compositional variability and possible deviations in homopause altitude between species. These findings underscore the importance of accounting for local atmospheric composition when interpreting ultraviolet auroral spectra and retrieving electron energy distributions.