  We report on interferometric observations with the CHARA Array of two
classical Wolf-Rayet stars in suspected binary systems, namely WR 137 and WR
138. In both cases, we resolve the component stars to be separated by a few
milliarcseconds. The data were collected in the H-band, and provide a measure
of the fractional flux for both stars in each system. We find that the WR star
is the dominant H-band light source in both systems ($f_{\rm WR, 137} =
0.59\pm0.04$; $f_{\rm WR, 138} = 0.67\pm0.01$), which is confirmed through both
comparisons with estimated fundamental parameters for WR stars and O dwarfs, as
well as through spectral modeling of each system. Our spectral modeling also
provides fundamental parameters for the stars and winds in these systems. The
results on WR 138 provide evidence that it is a binary system which may have
gone through a previous mass-transfer episode to create the WR star. The
separation and position of the stars in the WR 137 system together with
previous results from the IOTA interferometer provides evidence that the binary
is seen nearly edge-on. The possible edge-on orbit of WR 137 aligns well with
the dust production site imaged by the Hubble Space Telescope during a previous
periastron passage, showing that the dust production may be concentrated in the
orbital plane.
