We have carried out VLA imaging and a Fermi timing analysis of the 115 ms \gamma -ray and radio pulsar PSR J0002+6216 .
We found that the pulsar lies at the apex of a narrowly collimated cometary-like 7 ^ { \prime } tail of non-thermal radio emission which we identify as a bow-shock pulsar wind nebula .
The tail of the nebula points back toward the geometric center of the supernova remnant CTB 1 ( G116.9+0.2 ) 28 ^ { \prime } away , at a position angle \theta _ { \mu } = 113 ^ { \circ } .
We measure a proper motion with 2.9 \sigma significance from a Fermi timing analysis giving \mu =115 \pm 33 mas yr ^ { -1 } and \theta _ { \mu } = 121 ^ { \circ } \pm { 13 } ^ { \circ } , corresponding to a large transverse pulsar velocity of 1100 km s ^ { -1 } at a distance of 2 kpc .
This proper motion is of the right magnitude and direction to support the claim that PSR J0002+6216 was born from the same supernova that produced CTB 1 .
We explore the implications for pulsar birth periods , asymmetric supernova explosions , and mechanisms for pulsar natal kick velocities .