[en] ESO 381 - 47 is an early-type galaxy with an extended H I disk. Galaxy Evolution Explorer (GALEX) and very deep optical images reveal a distinct stellar ring far outside the optical body with a diameter of ∼30 kpc, which has undergone recent star formation at 1.8 x 10^-4 M _sun yr^-1 kpc^-2, consistent with other new results which detect low-level star formation below the traditional Kennicutt relation in the outer parts of spiral galaxies. The morphology of this galaxy resembles the recently identified class of ultraviolet objects called extended ultraviolet disks, or XUV-disks. New H I observations of this galaxy taken at the ATCA and in the CnB array at the VLA show that the cold gas lies in an extended (diameter ∼90 kpc) ring around the central S0 galaxy. The H I data cube can be well modeled by a warped ring. The faint ionized gas in the inner parts of the galaxy is kinematically decoupled from the stars and instead appears to exhibit velocities consistent with the rotation of the H I ring at larger radius. The peak of the stellar ring, as seen in the optical and UV, is slightly displaced to the inside relative to the peak of the H I ring. We discuss the manner in which this offset could be caused by the propagation of a radial density wave through an existing stellar disk, perhaps triggered by a galaxy collision at the center of the disk, or possibly due to a spiral density wave set up at early times in a disk too hot to form a stellar bar. Gas accretion and resonance effects due to a bar which has since dissolved are also considered to explain the presence of the star-forming ring seen in the GALEX and deep optical data.