  The initial Galactic velocity vector for the recently discovered hyperbolic
asteroid 1I/'Oumuamua (A/2017 U1) is calculated for before its encounter with
our solar system. The latest orbit (JPL-13) shows that 'Oumuamua has
eccentricity > 1 at 944\sigma\, significance (1.19936 +- 0.00021), i.e. clearly
unbound. Assuming no non-gravitational forces, the object's inbound Galactic
velocity was U, V, W = -11.457, -22.395, -7.746 (+-0.009, +-0.009, +-0.011)
km/s (U towards Galactic center), with total heliocentric speed 26.32 +- 0.01
km/s. When the velocity is compared to the local stars, 'Oumuamua can be ruled
out as co-moving with any of the dozen nearest systems, i.e. it does not appear
to be associated with any local exo-Oort clouds (most notably that of the Alpha
Centauri triple system). 'Oumuamua's velocity is within 5 km/s of the median
Galactic velocity of the stars in the solar neighborhood (<25 pc), and within 2
km/s of the mean velocity of the local M dwarfs. Its velocity appears to be
statistically "too" typical for a body whose velocity was drawn from the
Galactic velocity distribution of the local stars (i.e. less than 1 in 500
field stars in the solar neighborhood would have a velocity so close to the
median UVW velocity). In the Local Standard of Rest frame (circular Galactic
motion), 'Oumuamua is remarkable for showing both negligible radial (U) and
vertical (W) motion, while having a slightly sub-Keplerian circular velocity
(V; by ~11 km/s). These calculations strengthen the interpretation that A/2017
U1 has a distant extrasolar origin, but not among the very nearest stars. Any
formation mechanism for this interstellar asteroid should account for the
coincidence of 'Oumuamua's velocity being so close to the LSR.
