2013MNRAS.431.2590B

We report on sensitive phase referenced and gated 1.4 GHz very long baseline interferometry (VLBI) radio observations of the pulsar PSR J0205+6449 in the young pulsar wind nebula 3C 58, made in 2007 and 2010. We employed a novel technique where the ∼ 105-m Green Bank telescope is used simultaneously to obtain single-dish data used to determine the pulsar's period as well as to obtain VLBI data, allowing the VLBI correlation to be gated synchronously with the pulse to increase the signal-to-noise ratio. The high timing noise of this young pulsar precludes the determination of the proper motion from the pulsar timing. We derive the position of the pulsar accurate at the milliarcsecond level, which is consistent with a re-determined position from the Chandra X-ray observations. We reject the original tentative optical identification of the pulsar by Shearer & Neustroev in 2008, but rather identify a different optical counterpart on their images, with R-band magnitude ∼ 24. We also determine an accurate proper motion for PSR J0205+6449 of (2.3±0.3) mas yr-1, corresponding to a projected velocity of only (35±6)kms-1 for a distance of 3.2 kpc, at position angle -38°. This projected velocity is quite low compared to the velocity dispersion of known pulsars of ∼ 200kms-1. Our measured proper motion does not suggest any particular kinematic age for the pulsar.