In this paper we report the mapping of H3+, C2H2, and CH4 as derived by an unexploited Galileo/Near‐Infrared Mapping Spectrometer (NIMS) data set. As previously observed, hydrocarbons emissions appear to be located in the internal part of the auroral main oval, where CH4 3 µm vibrational band intensity ratios suggest that nonthermal excitation mechanisms, such as auroral particle precipitation and/or Joule heating, are responsible for the observed emissions. Temperature estimation are in good agreement for the CH4‐emitting region on the hot spot, while the values obtained for H3+ are lower in comparison with Cassini/visual and infrared mapping spectrometer and ground‐based data. C2H2 emission overlaps the CH4 one only at higher latitudes >75°N, indicating that different energetic particles are at work inside the main oval polar ward. CH4 is also found on the northern section of the main oval (135°< longitude <190°, 60°< latitude <90°N). The present investigation results have implications on the Juno/Jovian InfraRed Auroral Mapper observation planning as well as on the codes that will be used to retrieve temperatures and densities of all the emitting species involved in the Jupiter auroral processes. Key Points Maps of H3+, C2H2, and CH4 as derived by unexploited Galileo/NIMS data H3+ and CH4 temperatures and column densities derived for specific mean spectra. H3+ temperatures lower than previously reported Hydrocarbons emissions overlap only for latitudes >75°N indicating different energies of impacting particles polar ward