  We present the first double-lined orbital solution for the close binary in
the GW Ori triple system. Using 12 epochs of infrared spectroscopy, we detected
the lines of both stars in the inner pair, previously known as single-lined
only. Our preliminary infrared orbital solution has an eccentricity of e = 0.21
+/- 0.10, a period of P = 241.15 +/- 0.72 days, and a mass ratio of q = 0.66
+/- 0.13. We find a larger semi-amplitude for the primary star, K1 = 6.57 +/-
1.00 km s^-1, with an infrared-only solution compared to K1 = 4.41 +/- 0.33 km
s^-1 with optical data from the literature, likely the result of line blending
and veiling in the optical. The component spectral types correspond to G3 and
K0 stars, with vsini values of 43 km s^-1 and 50 km s^-1, respectively. We
obtained a flux ratio of alpha = 0.58 +/- 0.14 in the H-band, allowing us to
estimate individual masses of 3.2 and 2.7 M_sun for the primary and secondary,
respectively, using evolutionary tracks. The tracks also yield a coeval age of
1 Myr for both components to within 1 sigma. GW Ori is surrounded by a
circumbinary/circumtriple disk. A tertiary component has been detected in
previous studies; however, we did not detect this component in our
near-infrared spectra, probably the result of its relative faintness and
blending in the absorption lines of these rapidly rotating stars. With these
results, GW Ori joins the small number of classical T Tauri, double-lined
spectroscopic binaries.
