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 degrees + 3 degrees. 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.