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We observed Jupiter four times over a full rotation (10 hrs) with theupgraded Karl G. Jansky Very Large Array (VLA) between December 2013 andDecember 2014. Preliminary results at 4-17 GHz were presented in de Pater etal. (2016); in the present paper we present the full data set at frequenciesbetween 3 and 37 GHz. Major findings are: (i) the radio-hot belt at8.5--11$^\circ$N latitude, near the interface between the North Equatorial Belt(NEB) and the Equatorial Zone (EZ) is prominent at all frequencies (3--37 GHz).Its location coincides with the southern latitudes of the NEB (7--17$^{\circ}$N). (ii) Longitude-smeared maps reveal belts and zones at all frequencies atlatitudes $\lesssim |20^\circ|$. The lowest brightness temperature is in the EZnear a latitude of 4$^\circ$N, and the NEB has the highest brightnesstemperature near 11$^\circ$N. The bright part of the NEB increases inlatitudinal extent (spreads towards the north) with deceasing frequency, i.e.,with depth into the atmosphere. In longitude-resolved maps, several belts, inparticular in the southern hemisphere, are not continuous along the latitudeline, but broken into small segments as if caused by an underlying wave. (iii)Model fits to longitude-smeared spectra are obtained at each latitude. Theseshow a high NH$_3$ abundance (volume mixing ratio $\sim 4 \times 10^{-4}$) inthe deep ($P>8-10$ bar) atmosphere, decreasing at higher altitudes due to cloudformation (e.g., in zones), or dynamics in combination with cloud condensation(belts). In the NEB ammonia gas is depleted down to at least the 20 bar levelwith an abundance of $1.75 \times 10^{-4}$. (iv) Using the entire VLA dataset,we confirm that the planet is extremely dynamic in the upper layers of theatmosphere, at $P<$2--3 bar, i.e., at the altitudes where clouds form.[Abridged]

Jupiter's Ammonia Distribution Derived from VLA Maps at 3--37 GHz