1999ApJ...518..450P

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.