Results are presented from a long-term astrometry program on PSR B0919+06 using the NRAO Very Long Baseline Array .
With ten observations ( seven epochs ) between 1994–2000 , we measure a proper motion \mu _ { \alpha } = 18.35 \pm 0.06 mas yr ^ { -1 } , \mu _ { \delta } = 86.56 \pm 0.12 mas yr ^ { -1 } , and a parallax \pi = 0.83 \pm 0.13 mas ( 68 % confidence intervals ) .
This yields a pulsar distance of 1.21 \pm 0.19 kpc , making PSR B0919+06 the farthest pulsar for which a trigonometric parallax has been obtained , and the implied pulsar transverse speed is 505 \pm 80 km s ^ { -1 } .
Combining the distance estimate with interstellar scintillation data spanning 20 years , we infer the existence of a patchy or clumpy scattering screen along the line of sight in addition to the distributed electron density predicted by models for the Galaxy , and constrain the location of this scattering region to within \sim 250 parsecs of the Sun .
Comparison with the lines of sight towards other pulsars in the same quadrant of the Galaxy permits refinement of our knowledge of the local interstellar matter in this direction .