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We report low resolution near infrared spectroscopic observations of theeruptive star FU Orionis using the Integral Field Spectrograph Project 1640installed at the Palomar Hale telescope. This work focuses on elucidating thenature of the faint source, located 0.5" south of FU Ori, and identified in2003 as FU Ori S. We first use our observations in conjunction with publisheddata to demonstrate that the two stars are indeed physically associated andform a true binary pair. We then proceed to extract J and H bandspectro-photometry using the damped LOCI algorithm, a reduction method tailoredfor high contrast science with IFS. This is the first communication reportingthe high accuracy of this technique, pioneered by the Project 1640 team, on afaint astronomical source. We use our low resolution near infrared spectrum inconjunction with 10.2 micron interferometric data to constrain the infraredexcess of FU Ori S. We then focus on estimating the bulk physical properties ofFU Ori S. Our models lead to estimates of an object heavily reddened, A_V=8-12, with an effective temperature of ~ 4000-6500 K . Finally we put theseresults in the context of the FU Ori N-S system and argue that our analysisprovides evidence that FU Ori S might be the more massive component of thisbinary system

Constraining mass ratio and extinction in the FU Orionis binary system with infrared integral field spectroscopy