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We present the first double-lined orbital solution for the close binary inthe GW Ori triple system. Using 12 epochs of infrared spectroscopy, we detectedthe lines of both stars in the inner pair, previously known as single-linedonly. 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 kms^-1 with optical data from the literature, likely the result of line blendingand veiling in the optical. The component spectral types correspond to G3 andK0 stars, with vsini values of 43 km s^-1 and 50 km s^-1, respectively. Weobtained a flux ratio of alpha = 0.58 +/- 0.14 in the H-band, allowing us toestimate 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 of1 Myr for both components to within 1 sigma. GW Ori is surrounded by acircumbinary/circumtriple disk. A tertiary component has been detected inprevious studies; however, we did not detect this component in ournear-infrared spectra, probably the result of its relative faintness andblending in the absorption lines of these rapidly rotating stars. With theseresults, GW Ori joins the small number of classical T Tauri, double-linedspectroscopic binaries.

Orbital Solution for the Spectroscopic Binary in the GW Ori Hierarchical Triple