Multiple high-dispersion IUE spectra of SK159 in the Small Magellanic Cloud (SMC) have been obtained and averaged in order to study interstellar gas associated with the SMC and, in particular, to search for evidence of SMC halo gas. A single high-dispersion IUE spectrum of SK159 was analyzed by Prévot et al. (1980). They reported the absence of C IV and only the marginal detection of Si IV at SMC velocities. The higher signal-to-noise ratio in our data allow a more definitive investigation of the absorption characteristics of these ions. SK159 is relatively cool, spectral type BO.5 Iaw (Walborn 1983) and is located in a region free of strong nebulosity. Thus the interstellar line spectrum will be less contaminated by H II region absorption than in previous studies of SMC stars. This favorable circumstance is somewhat offset by the great complexity of the underlying stellar spectrum and the resultant blending of stellar and interstellar lines.