  We present new high-resolution radio and X-ray observations of the supernova
remnant (SNR) B0453-685 in the Large Magellanic Cloud, carried out with the
Australia Telescope Compact Array and the Chandra X-ray Observatory
respectively. Embedded in the SNR shell is a compact central nebula producing
both flat-spectrum polarized radio emission and non-thermal X-rays; we identify
this source as a pulsar wind nebula (PWN) powered by an unseen central neutron
star. We present a new approach by which the properties of a SNR and PWN can be
used to infer upper limits on the initial spin period and surface magnetic
field of the unseen pulsar, and conclude that this star was an initial rapid
rotator with current properties similar to those of the Vela pulsar. As is the
case for other similarly-aged sources, there is currently an interaction taking
place between the PWN and the SNR's reverse shock.
