Lunar and Planetary Science XXXVII (2006) 1564.pdf The JIRAM (Jovian InfraRed Auroral Mapper) Experiment. A. Coradini1 , A. Adriani1, G. Filacchione2, J.Lunine1,3, G. Magni2 , M. Cosi4 and L. Tommasi4, 1 INAF-IFSI, Via Fosso del Cavaliere, 100, Rome, Italy,
[email protected], 2INAF-IASF, Via Fosso del Cavaliere, 100, 00133, Rome, Italy, 3Lunar and Pla- netary Lab, University of Arizona, Tucson, AZ, USA, 4 Selex-Galileo Avionica, Via Albert Einstein 35, 50013 Campi Bisenzio (FI), Italy. + Introduction: The atmosphere of Jupiter requires aurora, the H3 is optimal for study. This molecule is multiple techniques at a variety of wavelengths. The formed at the base of the exosphere through the reac- + + present Juno payload is well-suited to a study of the tion H2 + H2 → H3 + H. The main roto-vibrational magnetic field and interior structure of Jupiter, as well band is around 4 µm and it is composed of more than as its plasma environment, but it will be strongly im- 200 possible transitions in the range 3.0 to 4.5 µm [1]. + proved by adding the capability to (a) image and make The H3 auroral spectrum was observed by Cassini spectra with high contrast of the Jovian aurora and (b) VIMS from a large distance in 2000, at much lower explore the region between roughly 1-10 bars where spatial resolution and signal-to-noise than that poten- water—Jupiter’s principal condensable because of the tially available from JIRAM. Figure 1 shows the capa- relatively high interior abundance of oxygen and ap- bility of imaging spectrometers to obtain excellent data propriate conditions in the 1-10 bar region—forms on emission features from which time-variability and clouds and aids energy transport by moist convection.