  We present the first kinematic study of extraplanar diffuse ionized gas
(eDIG) in the nearby, face-on disk galaxy M83 using optical emission-line
spectroscopy from the Robert Stobie Spectrograph on the Southern African Large
Telescope. We use a Markov Chain Monte Carlo method to decompose the
[NII]$\lambda\lambda$6548, 6583, H$\alpha$, and [SII]$\lambda\lambda$6717, 6731
emission lines into HII region and diffuse ionized gas emission. Extraplanar,
diffuse gas is distinguished by its emission-line ratios
([NII]$\lambda$6583/H$\alpha \gtrsim 1.0$) and its rotational velocity lag with
respect to the disk ($\Delta v = -24$ km/s in projection). With interesting
implications for isotropy, the velocity dispersion of the diffuse gas, $\sigma
= 96$ km/s, is a factor of a few higher in M83 than in the Milky Way and
nearby, edge-on disk galaxies. The turbulent pressure gradient is sufficient to
support the eDIG layer in dynamical equilibrium at an electron scale height of
$h_{z} = 1$ kpc. However, this dynamical equilibrium model must be finely tuned
to reproduce the rotational velocity lag. There is evidence of local bulk flows
near star-forming regions in the disk, suggesting that the dynamical state of
the gas may be intermediate between a dynamical equilibrium and a galactic
fountain flow. As one of the first efforts to study eDIG kinematics in a
face-on galaxy, this study demonstrates the feasibility of characterizing the
radial distribution, bulk velocities, and vertical velocity dispersions in
low-inclination systems.
