  The corona is an integral component of Active Galactic Nuclei (AGN) which
produces the bulk of the X-ray emission above 1--2 keV. However, many of its
physical properties and the mechanisms powering this emission remain a mystery.
In particular, the temperature of the coronal plasma has been difficult to
constrain for large samples of AGN, as constraints require high quality
broadband X-ray spectral coverage extending above 10 keV in order to measure
the high energy cutoff, which provides constraints on the combination of
coronal optical depth and temperature. We present constraints on the coronal
temperature for a large sample of Seyfert 1 AGN selected from the Swift/BAT
survey using high quality hard X-ray data from the NuSTAR observatory combined
with simultaneous soft X-ray data from Swift/XRT or XMM-Newton. When applying a
physically-motivated, non-relativistic disk reflection model to the X-ray
spectra, we find a mean coronal temperature kT $=$ 84$\pm$9 keV. We find no
significant correlation between the coronal cutoff energy and accretion
parameters such as the Eddington ratio and black hole mass. We also do not find
a statistically significant correlation between the X-ray photon index,
$\Gamma$, and Eddington ratio. This calls into question the use of such
relations to infer properties of supermassive black hole systems.
