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The vertical distribution of trace gases in planetary atmospheres can beobtained with observations of the atmosphere's thermal emission. Invertingradio observations to recover the atmospheric structure, however, isnon-trivial, and the solutions are degenerate. We propose a modeling frameworkto prescribe a vertical distribution of trace gases that combines athermo-chemical equilibrium model {based on a vertical temperature structureand compare these results to models where ammonia can vary between pre-definedpressure nodes}. To this means we retrieve nadir brightness temperatures andlimb-darkening parameters, together with their uncertainties, from the JunoMicrowave Radiometer (MWR). We then apply this framework to MWR observationsduring Juno's first year of operation (Perijove passes 1 - 12) and tolongitudinally-averaged latitude scans taken with the upgraded Very Large Array(VLA) (de Pater 2016,2019a). We use the model to constrain the distribution ofammonia between -60$^{\circ}$ and 60$^{\circ}$ latitude and down to 100 bar. Weconstrain the ammonia abundance to be $340.5^{+34.8}_{-21.2}$ ppm($2.30^{+0.24}_{-0.14} \times$ solar abundance), and find a depletion ofammonia down to a depth of $\sim$ 20 bar, which supports the existence ofprocesses that deplete the atmosphere below the ammonia and water cloud layers.At the equator we find an increase of ammonia with altitude, while the zonesand belts in the mid-latitudes can be traced down to levels where theatmosphere is well-mixed. The latitudinal variation in the ammonia abundanceappears to be opposite to that shown at higher altitudes, which supports theexistence of a stacked-cell circulation model.

Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter