  Recent surveys of the Magellanic Clouds have revealed a subtype of Wolf-Rayet
(WR) star with peculiar properties. WN3/O3 spectra exhibit both WR-like
emission and O3 V-like absorption - but at lower luminosity than O3 V or WN
stars. We examine the projected spatial distribution of WN3/O3 stars in the LMC
as compared to O-type stars. Surprisingly, WN3/O3 stars are among the most
isolated of all classes of massive stars; they have a distribution similar to
red supergiants dominated by initial masses of 10-15 $M_{\odot}$, and are far
more dispersed than classical WR stars or luminous blue variables (LBVs). Their
lack of association with clusters of O-type stars suggests strongly that WN3/O3
stars are not the descendants of single massive stars (30 $M_{\odot}$ or
above). Instead, they are likely products of interacting binaries at lower
initial mass (10-18 $M_{\odot}$). Comparison with binary models suggests a
probable origin with primaries in this mass range that were stripped of their H
envelopes through non-conservative mass transfer by a low-mass secondary. We
show that model spectra and positions on the Hertzsprung-Russell diagram for
binary stripped stars are consistent with WN3/O3 stars. Monitoring radial
velocities with high-resolution spectra can test for low-mass companions or
runaway velocities. With lower initial mass and environments that avoid very
massive stars, the WN3/O3 stars fit expectations for progenitors of Type Ib and
possibly Type Ibn supernovae.
