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We present the results from an optical spectroscopic analysis of the massivestars HD 37366 and HD 54662. We find that HD 37366 is a double-linedspectroscopic binary with a period of 31.8187 +/- 0.0004 days, and HD 54662 isalso a double lined binary with a much longer period of 557.8 +/- 0.3 days. Theprimary of HD 37366 is classified as O9.5 V, and it contributes approximatelytwo-thirds of the optical flux. The less luminous secondary is a broad-lined,early B-type main-sequence star. Tomographic reconstruction of the individualspectra of HD 37366 reveals absorption lines present in each component,enabling us to constrain the nature of the secondary and physicalcharacteristics of both stars. Tomographic reconstruction was not possible forHD 54662; however, we do present mean spectra from our observations that showthat the secondary component is approximately half as bright as the primary.The observed spectral energy distributions (SEDs) were fit with model SEDs andgalactic reddening curves to determine the angular sizes of the stars. Byassuming radii appropriate for their classifications, we determine distanceranges of 1.4 - 1.9 and 1.2 - 1.5 kpc for HD 37366 and HD 54662, respectively.

The Long Period, Massive Binaries HD 37366 and HD 54662: Potential Targets for Long Baseline Optical Interferometry