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    PR # 32125                                                                   
     Composite supernova remnants are the relatively small class of              
     remnants which display the expected result of a massive star                
     explosion: a central synchrotron nebula powered by a young neutron          
     star, and an expanding shell of emission produced by the stellar            
     ejecta. We propose to observe the two such objects at the extremes of       
     the radio synchrotron core luminosity distribution in order to              
     address such questions as the range of initial pulsar spin periods          
     and magnetic fields, as well as to establish the nebular spectral           
     break frequencies which reveal confinement pressures and field              
     strengths.                                                                  
                                                                                 
                                                                                 
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