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 arcmin 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 arcmin 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.
Categories: astro-ph.HE astro-ph.SR