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MWC 314 is one of the most luminous stars in the Milky Way. Its fundamentalparameters are similar to those of LBVs, although no large photometricvariations have been recorded.  We analyzed the radial velocity (RV) variations displayed by the absorptionlines from the star's atmosphere using high resolution optical spectra. The RVand profile variations of some permitted and forbidden emission lines ofmetallic ions and the behavior of the Balmer and HeI lines has beeninvestigated as well.  The RV of the absorption lines clearly shows a 60-day periodicity. A densecoverage of the RV curve allowed us to derive accurate orbital parameters. TheRV of the FeII emission lines varies in the same way, but with a smalleramplitude. Additionally, the intensity ratio of the blue/red peaks of theseemission lines correlates with the RV variations. The Balmer lines and {NII]lines display a nearly constant RV and no profile variations in phase with theorbital motion instead. The HeI-5876 \AA\ line shows a strongly variableprofile with broad and blue-shifted absorption components reaching velocitiesof <-1000 km/s at some specific orbital phases. Our data strongly suggest thatthe object is a binary system composed from a supergiant B[e] star and anundetected companion. The emission lines with a non-variable RV could originatein a circumbinary region. For the FeII emission lines we propose a simplegeometrical two-component model where a compact source of FeII emission, movingaround the center of mass, is affected by a static extra absorption thatoriginates from a larger area. Finally, the blue-shifted absorption in theHeI-5876 \AA\ line could be the result of density enhancements in the primarystar wind flowing towards the companion that is best observed when projectedover the disk of the primary star.

Interpreting the spectral behavior of MWC 314