  We observed Jupiter at wavelengths near 2 cm with the Karl G. Jansky Very
Large Array in February 2015. These frequencies are mostly sensitive to
variations in ammonia abundance and probe between ~0.5-2.0 bars of pressure in
Jupiter's atmosphere; within and below the visible cloud deck which has its
base near 0.7 bars. The resultant observed data were projected into a
cylindrical map of the planet with spatial resolution of ~1500 km at the
equator. We have examined the data for atmospheric waves and observed a
prominent bright belt of radio hotspot features near 10N, likely connected to
the same equatorial wave associated with the 5-micron hotspots. We conducted a
passive tracer power spectral wave analysis for the entire map. The power
spectra analysis revealed that the atmosphere sampled in our observation
(excluding the NEB region) is in a 2-D turbulent regime and its dynamics are
predominately governed by the shallow water equations. The GRS is also very
prominent and has a noticeable meridional asymmetry and we compare it, and
nearby storms, with optical images. We find that the meridional radio profile
has a global north-south hemisphere distinction and find correlations of it to
optical intensity banding and to shear zones of the zonal wind profile over
select regions of latitude. Amateur optical images taken before and after our
observation complemented the radio wavelength map to investigate dynamics of
the equatorial region in Jupiter's atmosphere. We find that two radio hotspots
at 2 cm are well correlated with optical plumes in the NEB, additionally
revealing they are not the same 5 micron hotspot features correlated with
optical dark patches between adjacent plumes. This analysis exploits the VLA's
upgraded sensitivity and explores the opportunities now possible when studying
gas giants, especially atmospheric dynamics of layers beneath upper level
clouds.
