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We have obtained high-resolution spectra of Jupiter's Great Red Spot (GRS)between 4.6 and 5.4 microns using telescopes on Mauna Kea in order to derivegas abundances and to constrain its cloud structure between 0.5 and 5~bars. Weused line profiles of deuterated methane CH3D at 4.66 microns to infer thepresence of an opaque cloud at 5+/-1 bar. From thermochemical models this isalmost certainly a water cloud. We also used the strength of Fraunhofer linesin the GRS to obtain the ratio of reflected sunlight to thermal emission. Thelevel of the reflecting layer was constrained to be at 570+/-30 mbar based onfitting strong ammonia lines at 5.32 microns. We identify this layer as anammonia cloud based on the temperature where gaseous ammonia condenses. Wefound evidence for a strongly absorbing, but not totally opaque, cloud layer atpressures deeper than 1.3 bar by combining Cassini/CIRS spectra of the GRS at7.18 microns with ground-based spectra at 5 microns. This is consistent withthe predicted level of an NH4SH cloud. We also constrained the vertical profileof water and ammonia. The GRS spectrum is matched by a saturated water profileabove an opaque water cloud at 5~bars. The pressure of the water cloudconstrains Jupiter's O/H ratio to be at least 1.1 times solar. The ammonia molefraction is 200+/-50ppm for pressures between 0.7 and 5 bar. Its abundance is40 ppm at the estimated pressure of the reflecting layer. We obtained 0.8+/-0.2ppm for PH3, a factor of 2 higher than in the warm collar surrounding the GRS.We detected all 5 naturally occurring isotopes of germanium in GeH4 in theGreat Red Spot. We obtained an average value of 0.35+/-0.05 ppb for GeH4.Finally, we measured 0.8+/-0.2 ppb for CO in the deep atmosphere.

The Gas Composition and Deep Cloud Structure of Jupiter's Great Red Spot