  We report astrometric results of phase-referencing VLBI observations of 43
GHz SiO maser emission toward the red hypergiant VY Canis Majoris (\vycma)
using the Very Long Baseline Array (VLBA). We measured a trigonometric parallax
of 0.83 $\pm$ 0.08 mas, corresponding to a distance of 1.20$^{+0.13}_{-0.10}$
kpc. Compared to previous studies, the spatial distribution of SiO masers has
changed dramatically, while its total extent remains similar. The internal
motions of the maser spots are up to 1.4 \masy, corresponding to 8 \kms, and
show a tendency for expansion. After modeling the expansion of maser spots, we
derived an absolute proper motion for the central star of \mux\ = $-2.8 \pm
0.2$ and \muy\ = $2.6 \pm 0.2$ \masy\ eastward and northward, respectively.
Based on the maser distribution from the VLBA observations, and the relative
position between the radio photosphere and the SiO maser emission at 43 GHz
from the complementary Very Large Array (VLA) observations, we estimate the
absolute position of \vycma\ at mean epoch 2006.53 to be \ra\ = 07\h 22\m
58\decs3259 $\pm$ 0\decs0007, \dec\ = $-$25\arcdeg 46\arcmin03\decas063 $\pm$
0\decas010. The position and proper motion of \vycma\ from the VLBA
observations differ significantly with values measured by the Hipparcos
satellite. These discrepancies are most likely associated with inhomogeneities
and dust scattering the optical light in the circumstellar envelope. The
absolute proper motion measured with VLBA suggests that \vycma\ may be drifting
out of the giant molecular cloud to the east of it.
