Tomographic Separation of Composite Spectra. VI. The Physical Properties of the Massive Close Binary HD 152248

We present the results of a Doppler tomographic reconstruction of the UV spectra of the double-lined O binary HD 152248 based on observations made with IUE . We used cross-correlation methods to obtain radial velocities, confirm the orbital elements, estimate the UV flux ratio, and determine projected rotational velocities. The individual component spectra are classified as O7 I + O7 I using UV criteria defined by Penny, Gies, & Bagnuolo. We present a model fit of the eclipsing light curve from which we derive an orbital inclination, i =72° ± 3°. This analysis indicates that neither star is currently experiencing Roche lobe overflow. We place the individual components in the theoretical H-R diagram and show that the individual masses ( M p / M ☉ =24.2 ± 2.0; M s / M ☉ =25.8 ± 2.0) derived from the combined spectroscopic and photometric analysis are significantly lower than those computed from evolutionary tracks for single stars.