  As part of a multi-year survey for Wolf-Rayet stars in the Magellanic Clouds,
we have discovered a new type of Wolf-Rayet star with both strong emission and
absorption. While one might initially classify these stars as WN3+O3V binaries
based on their spectra, such a pairing is unlikely given their faint visual
magnitudes. Spectral modeling suggests effective temperatures and bolometric
luminosities similar to those of other early-type LMC WNs but with mass-loss
rates that are three to five times lower than expected. They additionally
retain a significant amount of hydrogen, with nitrogen at its CNO-equilibrium
value (10x enhanced). Their evolutionary status remains an open question. Here
we discuss why these stars did not evolve through quasi-homogeneous evolution.
Instead we suggest that based on a link with long-duration gamma ray bursts,
they may form in lower metallicity environments. A new survey in M33, which has
a large metallicity gradient, is underway.
