mbar pressure region and as a gaseous constituent above the clouds up to the tropopause (Θ150 mbar). The presence We report results from measurements of NH 3 emission lines from the stratosphere of Jupiter following the impacts of frag-of gaseous ammonia in the troposphere is evidenced by ments of Comet P/Shoemaker-Levy 9. Measurements were prominent absorption spectra which have been measured taken at the NASA Infrared Telescope Facility on 29 July 1994 on Jupiter in the thermal infrared spectral region by the on two impact regions, Q1 and the RSG complex, Θ8 days Voyager infrared interferometer spectrometer, IRIS, after the impacts. Emission line profiles were obtained near (Kunde et al. 1982). 11.2 m at sub-Doppler spectral resolution (/β¬ Θ 10 6 ). The Ammonia is not normally found in Jupiter's stratomeasurements of the lineshapes permit the retrieval of NH 3 sphere. Photochemical models for ammonia on Jupiter abundance and provide constraints on its altitude distribution have been developed (Atreya et al. 1977, Kaye and Strobel in the stratosphere. If a uniformly mixed altitude distribution 1983) which indicate that this depletion is due to rapid is assumed above the tropopause, the retrieved NH 3 mole fracphotolysis by solar UV radiation and condensation at the tions are 7.8 Ψ 1.6 Ψ 10 Ψ9 for the Q1 impact region and 4 Ψ tropopause. The Comet Shoemaker-Levy 9 collision event 0.8 Ψ 10 Ψ9 for the RSG impact region. The total derived mass of NH 3 , Θ4 Ψ 10 12 g within our field of view, is approximately on Jupiter provided a unique opportunity to study the 20 times greater than that possible from cometary origin. Near lifetime of NH 3 in Jupiter's stratosphere and to constrain the Q1 impact site, ammonia emission is found to originate existing photochemical models (Moses et al. 1995). The primarily from altitudes above the 10 mbar level, with a mole fact that NH 3 was found in the stratosphere in significant fraction of 18 Ψ 4 Ψ 10 Ψ9 corresponding to a column abundance abundance after the collision events (cf. Orton et al. 1995, of 2 Ψ 0.4 Ψ 10 16 cm Ψ2 . Results are compared with other infrared Noll et al. 1995) also provides information on the depth and ultraviolet measurements and with recent photochemical of penetration and the energy of the individual fragments. models for jovian stratospheric NH 3 . These comparisons pro-As the fragments of Comet SL9 entered Jupiter's atmovide evidence for the presence of haze up to the 10 mbar level sphere, many penetrated into the deep atmosphere at or and provide an initial data set for study of the temporal behavior below the NH 3 cloud level. The resultant fireball and fallof NH 3 in the stratosphere of Jupiter.