  High time resolution observations of PSR B0906-49 (or PSR J0908-4913) over a
wide range of frequencies have enabled us to determine the geometry and beam
shape of the pulsar. We have used the position angle traverse to determine
highly-constrained solutions to the rotating vector model which show
conclusively that PSR B0906-49 is an orthogonal rotator. The accuracy obtained
in measuring the geometry is unprecedented. This may allow tests of high-energy
emission models, should the pulsar be detected with GLAST. Although the impact
parameter, beta, appears to be frequency dependent, we have shown that this is
due to the effect of interstellar scattering. As a result, this pulsar provides
some of the strongest evidence yet that the position angle swing is indeed
related to a geometrical origin, at least for non-recycled pulsars. We show
that the beam structures of the main pulse and interpulse in PSR B0906-49 are
remarkably similar. The emission comes from a height of ~230 km and is
consistent with originating in a patchy cone located about half way to the last
open field lines. The rotation axis and direction of motion of the pulsar
appear to be aligned.
