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 \emph { e } = 0.21 \pm 0.10 , a period of P = 241.15 \pm 0.72 days , and a mass ratio of q = 0.66 \pm 0.13 .
We find a larger semi-amplitude for the primary star , K 1 = 6.57 \pm 1.00 km s ^ { -1 } , with an infrared-only solution compared to K 1 = 4.41 \pm 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 v \sin i values of 43 km s ^ { -1 } and 50 km s ^ { -1 } , respectively .
We obtained a flux ratio of \alpha = 0.58 \pm 0.14 in the H-band , allowing us to estimate individual masses of 3.2 and 2.7 M _ { \odot } 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 .