  The vertical distribution of trace gases in planetary atmospheres can be
obtained with observations of the atmosphere's thermal emission. Inverting
radio observations to recover the atmospheric structure, however, is
non-trivial, and the solutions are degenerate. We propose a modeling framework
to prescribe a vertical distribution of trace gases that combines a
thermo-chemical equilibrium model {based on a vertical temperature structure
and compare these results to models where ammonia can vary between pre-defined
pressure nodes}. To this means we retrieve nadir brightness temperatures and
limb-darkening parameters, together with their uncertainties, from the Juno
Microwave Radiometer (MWR). We then apply this framework to MWR observations
during Juno's first year of operation (Perijove passes 1 - 12) and to
longitudinally-averaged latitude scans taken with the upgraded Very Large Array
(VLA) (de Pater 2016,2019a). We use the model to constrain the distribution of
ammonia between -60$^{\circ}$ and 60$^{\circ}$ latitude and down to 100 bar. We
constrain 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 of
ammonia down to a depth of $\sim$ 20 bar, which supports the existence of
processes that deplete the atmosphere below the ammonia and water cloud layers.
At the equator we find an increase of ammonia with altitude, while the zones
and belts in the mid-latitudes can be traced down to levels where the
atmosphere is well-mixed. The latitudinal variation in the ammonia abundance
appears to be opposite to that shown at higher altitudes, which supports the
existence of a stacked-cell circulation model.
