  We present ultraviolet and optical spectra of DI 1388, a young star in the
Magellanic Bridge, a region of gas between the Small and Large Magellanic
Clouds. The data have signal-to-noise ratios of 20 to 45 and a spectral
resolution of 6.5 km/s. Interstellar absorption by the Magellanic Bridge at
v_LSR = 200 km/s is visible in the lines of C I, C II,C II*, C IV, N I, O I, Al
II, Si II, Si III, Si IV, S II, Ca II, Fe II, and Ni II. The relative gas-phase
abundances of C II, N I, O I, Al II, Si II, Fe II, and Ni II with respect to S
II are similar to those found in Galactic halo clouds, despite a significantly
lower metallicity in the Magellanic Bridge. The higher ionization species in
the cloud have a column density ratio N(C IV)/N(Si IV) about 1.9, similar to
that inferred for collisionally ionized Galactic cloud interfaces at
temperatures 10^5 K.We identify sub-structure in the stronger interstellar
lines, with a broad component (FWHM = 20 km/s) at 179 km/s and a sharp
component (FWHM = 11 km/s) at 198 km/s. The abundance analysis for these clouds
indicates that the feature at 198 km/s consists of a low electron density,
mainly neutral gas that may be associated with an interface responsible for the
highly ionized gas. The 179 km/s cloud consists of warmer, lower density gas
that is partially ionized.
