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be identified with periodic features such as vortex chains and the equatorial plumes. The origin of others is less certain. WeWe study power spectra and search for planetary waves in present a table of our best wave candidates. 1996 Academic Press, Inc.images of Jupiter’s cloud opacity. The observation wavelength of 4.9 mm senses thermal emission from the p5-bar level; overly-ing clouds attenuate the emission. Our companion paper (J. INTRODUCTIONHarrington, T. E. Dowling, and R. L. Baron, 1996, Icarus 124, 22–31) describes 19 nights of observations (6 with 3608 longi-Jupiter’s middle and deep atmospheric regions stronglytude coverage) and new reduction techniques. Atmospheric influence the types of dynamics that occur above themseeing limits resolution to p2500 km. Zonal power spectral density at planetary wavenumbers higher than p25 follows a (Dowling and Ingersoll 1989). The direct study of thes