emit over nearly the entire electromagnetic spectrum, and multiwavelength observations have become an important source of physical information about the ejecta (in young objects), and the circumstellar medium and ISM into which the shock wave propagates.

Ultraviolet spectroscopy of SNRs has proven to be an important tool for providing physical information and insight into this important class of objects (Blair 2001; Raymond 2001; and references therein). Emission lines in the UV tend to come from material at temperatures that are intermediate between the X-ray emitting gas and the optical filaments. Information on shock velocities, preshock densities, and abundances of important elements such as carbon that have no bright optical lines can all be derived from UV observations of shocks. $\fuse$ observations have the added bonus of high spectral resolution, which provides kinematic and line profile information. Thus the importance of overlying absorption and in some cases the shock geometry can be assessed directly (Blair, Sankrit, & Tulin 2002; Sankrit, Blair, & Raymond 2003).

Primarily because of interstellar extinction, however, there are remarkably few objects available for study in the UV. In our Galaxy, the Cygnus Loop and Vela SNRs are the objects that have been studied extensively; both are nearby 