Far Ultraviolet Spectroscopic Explorer observations of a supernova remnantin the line of sight to HD 5980 in the Small Magellanic Cloud

We report a detection of far-ultraviolet absorption from the supernova remn ant SNR 0057-7226 in the Small Magellanic Cloud (SMC). The absorption is se en in the Far Ultraviolet Spectroscopic Explorer (FUSE) spectrum of the lum inous blue variable/Wolf-Rayet star HD 5980. Absorption from O vi lambda 10 32 and C III lambda 977 is seen at a velocity of 300 km s(-1) with respect to the Galactic absorption lines, 170 km s(-1) with respect to the SMC abso rption. The O vi lambda 1038 line is contaminated by H-2 absorption but is present. These lines are not seen in the FUSE spectrum of Sk 80, only simil ar to1' (similar to 17 pc) away from HD 5980. No blueshifted O vi lambda 10 32 absorption from the SNR is seen in the FUSE spectrum. The O vt lambda 10 32 line in the SNR is well described by a Gaussian with FWHM = 75 km s(-1). We find log N(O vi) = 14.33-14.43, which is roughly 50% of the rest of the O vi column in the SMC (excluding the SNR) and greater than the O vi colum n in the Milky Way halo along this sight line. The N(C iv)/N(O vi) ratio fo r the SNR absorption is in the range of 0.12-0.17, similar to the value see n in the Milky Way disk and lower than the halo value. supporting models in which SNRs produce the highly ionized gas close to the plane of the Galaxy , while other mechanisms occur in the halo. The N(C iv)/N(O vi) ratio is al so lower than the SMC ratio along this sight line, suggesting that other me chanisms contribute to the creation of the global hot ionized medium in the SMC. The O vi, C iv, and Si iv apparent column density profiles suggest th e presence of a multiphase shell followed by a region of higher temperature gas.