luminosities in O VI, based simply on scaling the flux at the observed positions to an entire object, span a broad range from considerably brighter to many times fainter than the inferred soft X-ray luminosities, indicating that O VI can be an important and largely unrecognized coolant in certain objects. We compare the optical and X-ray properties of the detected and non-detected objects but do not find a simple indicator for ultraviolet detectability. Non-detections may be due to clumpiness of the emission, high foreground extinction, slow shocks whose emission gets attenuated by the Magellanic interstellar medium, or a combination of these effects. The characteristics of individual detected supernova remnants are summarized in an Appendix.'
author:
- 'William P. Blair, Parviz Ghavamian, Ravi Sankrit, & Charles W. Danforth'
title: ' [*Far Ultraviolet Spectroscopic Explorer*]{} Survey of Magellanic Cloud Supernova Remnants'
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Introduction
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Supernova remnants (SNRs) as a class are important constituents of the interstellar medium (ISM). They are responsible for much of the enrichment of the ISM of a galaxy, and they are a significant energy source for stirring and mixing the ISM. They may also be important in some regions for triggering star formation in molecular clouds. SNRs typically 