  We present X-ray and radio observations of the recently-discovered bow shock
pulsar wind nebula associated with PSR J0002+6216, characterizing the PWN
morphology, which was unresolved in previous studies. The multi-frequency,
multi-epoch Very Large Array radio observations reveal a cometary tail trailing
the pulsar and extending up to 5.3', with multiple kinks along the emission.
The presented radio continuum images from multi-configuration broadband VLA
observations are one of the first results from the application of multi-term
multi-frequency synthesis deconvolution in combination with the awproject
gridder implemented in the Common Astronomy Software Applications package
(CASA). The X-ray emission observed with Chandra extends to only 21'', fades
quickly, and has some hot spots present along the extended radio emission.
These kinks could indicate the presence of density variation in the local ISM
or turbulence. The bow shock standoff distance estimates a small bow shock
region with a size 0.003-0.009 pc, consistent with the pulsar spin-down power
of Edot=1.51x10^35 ergs/s estimated from timing. The high-resolution radio
image reveals the presence of an asymmetry in the bow shock region which is
also present in the X-ray image. The broadband radio image shows an unusually
steep spectrum along with a flat-spectrum sheath, which could indicate varying
opacity or energy injection into the region. Spatially-resolved X-ray spectra
provide marginal evidence of synchrotron cooling along the extended tail. Our
analysis of the X-ray data also shows that this pulsar has a low spin-down
power and one of the lowest X-ray efficiencies observed in these objects.
