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We report the results of X-ray (CXO) and radio (ATCA) observations of thepulsar wind nebula (PWN) powered by the young pulsar PSR J1016--5857, which wedub "the Goose" PWN. In both bands the images reveal a tail-like PWN morphologywhich can be attributed to pulsar's motion. By comparing archival and new CXOobservations, we measure the pulsar's proper motion $\mu=28.8\pm7.3$ mas/yr,yielding a projected pulsar velocity $v \approx 440\pm110$ km/s (at d=3.2 kpc);its direction is consistent with the PWN shape. Radio emission from the PWN ispolarized, with the magnetic field oriented along the pulsar tail. The radiotail connects to a larger radio structure (not seen in X-rays) which weinterpret as a relic PWN (also known as a plerion). The spectral analysis ofthe CXO data shows that the PWN spectrum softens from $\Gamma=1.7$ to$\Gamma\approx2.3-2.5$ with increasing distance from the pulsar. The softeningcan be attributed to rapid synchrotron burn-off, which would explain the lackof X-ray emission from the older relic PWN. In addition to non-thermal PWNemission, we detected thermal emission from a hot plasma which we attribute tothe host SNR. The radio PWN morphology and the proper motion of the pulsarsuggest that the reverse shock passed through the pulsar's vicinity and pushedthe PWN to one side.

"The Goose" Pulsar Wind Nebula of PSR J1016-5857: The Birth of a Plerion