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The "Mouse" (PWN G359.23-0.82) is a spectacular bow shock pulsar wind nebula,powered by the radio pulsar J1747-2958. The pulsar and its nebula are presumedto have a high space velocity, but their proper motions have not been directlymeasured. Here we present 8.5 GHz interferometric observations of the Mousenebula with the Very Large Array, spanning a time baseline of 12 yr. We measureeastward proper motion for PWN G359.23-0.82 (and hence indirectly for PSRJ1747-2958) of 12.9+/-1.8 mas/yr, which at an assumed distance of 5 kpccorresponds to a transverse space velocity of 306+/-43 km/s. Consideringpressure balance at the apex of the bow shock, we calculate an in situ hydrogennumber density of approximately 1.0(-0.2)(+0.4) cm^(-3) for the interstellarmedium through which the system is traveling. A lower age limit for PSRJ1747-2958 of 163(-20)(+28) kyr is calculated by considering its potentialbirth site. The large discrepancy with the pulsar's spin-down age of 25 kyr ispossibly explained by surface dipole magnetic field growth on a timescale ~15kyr, suggesting possible future evolution of PSR J1747-2958 to a differentclass of neutron star. We also argue that the adjacent supernova remnantG359.1-0.5 is not physically associated with the Mouse system but is rather anunrelated object along the line of sight.

A Proper Motion for the Pulsar Wind Nebula G359.23-0.82, "the Mouse," Associated with the Energetic Radio Pulsar J1747-2958