With a period of 51.6 ms and spin-down power 2.2 \times 10 ^ { 37 } erg s ^ { -1 } , PSR J2229+6114 is a compelling identification for the EGRET source 3EG J2227+6122 in which error circle it resides . Striking features of the Chandra X-ray image are an incomplete elliptical arc and a possible jet , similar to the structures that dominate the appearance of the Vela PWN . Approximately 70 % of the 2–10 keV X-ray emission comes from a centrally peaked , diffuse nebula of radius 100 ^ { \prime \prime } with a power-law spectrum of photon index 1.45 \pm 0.19 . The pulsar itself has a marginally harder spectrum with photon index 0.99 \pm 0.27 . For an assumed distance of 3 kpc the ratio of X-ray luminosity to spin-down power of PSR J2229+6114 is only 8 \times 10 ^ { -5 } . We discuss a model in which such inefficient X-ray emission is the signature of a highly magnetized pulsar wind that prevents an internal MHD shock , at the location of the X-ray arc , from strongly compressing the flow . The incomplete X-ray arc is consistent with beaming from a relativistic equatorial outflow , while a surrounding radio shell is probably the forward shock in the surrounding ISM . An MeV source at this location was previously detected by the COMPTEL experiment on CGRO . This , plus the flat X-ray spectrum in the 2–10 keV band , suggests that PSR J2229+6114 is one of the brightest pulsars at 1 MeV , even while it is inconspicuous at radio through X-ray wavelengths , and as steep as the Crab above 100 MeV . The apparent variety of broad-band spectra displayed by high-energy pulsars bolsters the theory that rotation-powered pulsars dominate the unidentified Galactic EGRET source population .