  We report on Australia Telescope Compact Array observations in the direction
of the young high-magnetic-field radio pulsar PSR J1119-6127. In the resulting
images we identify a non-thermal radio shell of diameter 15 arcminutes, which
we classify as a previously uncataloged young supernova remnant (SNR),
G292.2-0.5. This SNR is positionally coincident with PSR J1119-6127, and we
conclude that the two objects are physically associated. No radio emission is
detected from any pulsar wind nebula (PWN) associated with the pulsar; our
observed upper limits are consistent with the expectation that
high-magnetic-field pulsars produce radio nebulae which fade rapidly. This
system suggests a possible explanation for the lack of associated radio pulsars
and/or PWNe in many SNRs.
