  We present the first visual orbit for the nitrogen-rich Wolf-Rayet binary, WR
133 (WN5o + O9I) based on observations made with the CHARA Array and the MIRC-X
combiner. This orbit represents the first visual orbit for a WN star and only
the third Wolf-Rayet star with a visual orbit. The orbit has a period of 112.8
d, a moderate eccentricity of 0.36, and a separation of $a$= 0.79 mas on the
sky. We combine the visual orbit with an SB2 orbit and Gaia parallax to find
that the derived masses of the component stars are $M_{\rm WR}$ = $9.3\pm1.6
M_\odot$ and $M_{\rm O}$ = $22.6\pm 3.2 M_\odot$, with the large errors owing
to the nearly face-on geometry of the system combined with errors in the
spectroscopic parameters. We also derive an orbital parallax that is identical
to the {\it Gaia}-determined distance. We present a preliminary spectral
analysis and atmosphere models of the component stars, and find the mass-loss
rate in agreement with polarization variability and our orbit. However, the
derived masses are low compared to the spectral types and spectral model. Given
the close binary nature, we suspect that WR 133 should have formed through
binary interactions, and represents an ideal target for testing evolutionary
models given its membership in the cluster NGC 6871.
