  We present a first look at the MRS observations of the nucleus of the nearby
galaxy M83, taken with MIRI onboard JWST. The observations show a rich set of
emission features from the ionized gas, warm molecular gas, and dust. To begin
dissecting the complex processes in this part of the galaxy, we divide the
observations into four different regions. We find that the strength of the
emission features varies strongly from region to region, with the south-east
region displaying the weakest features tracing the dust continuum and ISM
properties. Comparison between the cold molecular gas traced by the $^{12}$CO
(1-0) transition with ALMA and the H$_2$ S(1) transition shows a similar
spatial distribution. This is in contrast to the distribution of the much
warmer H$_2$ emission from the S(7) transition found to be concentrated around
the optical nucleus. We use the rotational emission lines and model the H$_2$
excitation to estimate a total molecular gas mass accounting for the warm H$_2$
component of M($>$50 K)$_{\rm H_{2}}$ = 67.90 ($\pm 5.43$)$\times$10$^{6}$
M$_{\odot}$. We compare this value to the total gas mass inferred by probing
the cold H$_2$ gas through the $^{12}$CO (1-0) emission, M(CO)$_{\rm H_{2}}$ =
17.15$\times$10$^{6}$ M$_{\odot}$. We estimate that $\sim$75\% of the total
molecular gas mass is contained in the warm H$_2$ component. We also identify
[\ion{O}{4}] 25.89 $\mu$m and [\ion{Fe}{2}] 25.99 $\mu$m emission. We propose
that the diffuse [\ion{Fe}{2}] 25.99 $\mu$m emission might be tracing shocks
created during the interactions between the hot wind produced by the starburst
and the much cooler ISM above the galactic plane. More detailed studies are
needed to confirm such a scenario.
