  We report our measurement of the trigonometric distance and proper motion
IRAS 20056+3350, obtained from the annual parallax of H2O masers. Our distance
of D = 4.69 +0.65-0.51 kpc, which is more than two times larger than the near
kinematic distance adopted in the literature, places IRAS 20056+3350 at the
leading tip of the Local arm, and proximal to the Solar circle. Using our
distance we re-evaluate past observations to reveal IRAS 20056+3350 as a site
of massive star formation at a young stage of evolution. This result is
consistent with the spectral energy distribution of the source evaluated with
published photometric data from UKIDSS, WISE, AKARI, IRAS and sub-millimetre
continuum. Both analytical approaches reveal the luminosity of the region to be
2.4 x 10^4 Lo, and suggest that IRAS 20056+3350 is forming an embedded star of
16 Mo. We estimated the proper motion of IRAS 20056+3350 to be
($\mu_{\alpha}\cos\delta$, $\mu_{\delta}$) = ($-2.62\pm0.33$, $-5.65\pm0.52$)
mas yr$^{-1}$ from the group motion of H$_{2}$O masers, and use our results to
estimate the angular velocity of Galactic rotation at the Galactocentric
distance of the Sun, $\Omega_{0} = 28.71\pm0.63$ km s$^{-1}$ kpc$^{-1}$, which
is consistent with the values obtained for other tangent point and Solar circle
objects.
