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We present the results of optical wavelength observations of the unusual SMCeclipsing binary system HD 5980 obtained in 1999 and 2004--2005. Radialvelocity curves for the erupting LBV/WR object (star A) and its close WR-likecompanion (star B) are obtained by deblending the variable emission-lineprofiles of N IV and N V lines under the simplistic assumption that these linesoriginate primarily in the winds of star A and star B. The derived massesM_A=58--79 Mo and M_B=51--67 Mo, are more consistent with the stars' locationnear the top of the HRD than previous estimates. The presence of a wind-windinteraction region is inferred from the orbital phase-dependent behavior of HeI P Cygni absorption components. The emission-line intensities continued withthe declining trend previously seen in UV spectra. The behavior of thephotospheric absorption lines is consistent with the results of Schweickhardt(2002) who concludes that the third object in the combined spectrum, star C, isalso a binary system with P(starC)~96.5 days, e=0.83. The data used in thispaper will be made publicly available for further analysis.

New insights into the nature of the SMC WR/LBV binary HD 5980