  N66/NGC346 is the largest and brightest HII region in the Small Magellanic
Cloud and contains at least one known supernova remnant SNR0057-7226. Optical
emission from the remnant is overwhelmed by the bright photoionized emission
from the nebula, but the remnant has been detected by way of far ultraviolet
absorption lines. Here we present data from the Far Ultraviolet Spectroscopic
Explorer (FUSE) satellite showing strong OVI and CIII emission from a position
at the edge of SNR0057-7226. We also present high-resolution, long-slit Halpha
spectra across N66 showing high- and low-velocity emission corresponding
closely to the X-ray boundaries of the supernova remnant. We use these FUV and
optical data to determine the physical parameters of the shock and interaction
geometry with N66. We find that ionizing photons from the many massive cluster
stars nearby likely affect the ionization balance in the post-shock gas,
hindering the production of lower-ionization and neutral species. We discuss
the importance and inherent difficulty of searching for supernova remnants in
or near bright HII regions and suggest that the far ultraviolet provides a
viable means to discover and study such remnants.
