  We perform an expansion study of the Balmer dominated outer shock of the SNR
0519$-$69.0 in the LMC by using a combination of new HST WFC3 imagery obtained
in 2020 and archival ACS images from 2010 and 2011. Thanks to the very long
time baseline, our proper motion measurements are of unprecedented accuracy. We
find a wide range of shock velocities, with the fastest shocks averaging 5280
km/s and the slowest grouping of shocks averaging just 1670 km/s. We compare
the H_alpha images from HST with X-ray images from Chandra and mid-IR images
from Spitzer, finding a clear anti-correlation between the brightness of the
remnant in a particular location and the velocity of the blast wave at that
location, supporting the idea that the bright knots of X-ray and IR emission
result from an interaction with a dense inhomogeneous circumstellar medium. We
find no evidence for X-ray emission, thermal or nonthermal, associated with the
fastest shocks, as expected if the fastest velocities are the result of the
blast wave encountering the lower density ambient medium of the LMC. We derive
an age of the remnant of 670 +/- 70 yr, consistent with results derived from
previous investigations.
