Conclusion

The unprecedented capabilities of XMM-Newton and Chandra (and ROSAT and ASCA before them) have led to important new insights into the astrophysics of supernova remnants. As these missions continue we can expect further new developments. Examples include direct expansion measurements in additional young SNRs and sensitive searches for trace elements. The new Suzaku Observatory with its sensitive Hard X-ray Detector will measure the spectra of the hard component in many SNRs and crudely map it for large remnants. High spectral resolution spatially resolved spectroscopy will someday allow detailed plasma diagnostics.

Much can be done for X-ray supernovae as well. The high sensitivity of XMM-Newton and Chandra allow the light curves of the known SNe to be tracked to much lower flux. Benefits include mapping of the pre-SN wind density to ever longer times, and further narrowing the observational gap between SNe and the historical SNRs. SN research in the X-rays, as in other bands, still relies primarily on serendipity, however. Fortunately, the Swift Observatory, with its rapid response to new phenomena, allows SNe to be observed in X-rays within hours of discovery and frequently monitored thereafter. Of course, it is the hope of all researchers in this field that before the end of these missions the opportunity arises to observe a new Galactic supernova.

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