THE AIM OF THIS PROPOSAL IS TO MAXIMIZE THE SCIENTIFIC RETURN OF EXISTING AND FUTURE MULTI-WAVELENGTH OBSERVATIONS OF THE SUPERNOVA REMNANTS (SNRS) FROM CORE COLLAPSE SUPERNOVAE (CCSNE). OUR MAIN DELIVERABLE WILL BE A GRID OF MODELS THAT WILL ALLOW THE COMMUNITY TO INTERPRET CC SNR OBSERVATIONS IN TERMS OF THE BASIC FEATURES OF CCSNE THE STELLAR EVOLUTION OF THEIR PROGENITORS AND THE PHYSICS OF SNR SHOCKS. TO PRODUCE THIS GRID OF MODELS WE WILL USE A CODE THAT FOLLOWS THE INTERACTION BETWEEN THE CCSN EJECTA AND THE CIRCUMSTELLAR MEDIUM (CSM) MODIFIED BY THEIR MASSIVE PROGENITORS INCLUDING TIME-DEPENDENT NONEQUILIBRIUM IONIZATION (NEI) RADIATIVE LOSSES AND A DETAILED TREATMENT OF COSMIC RAY (CR) ACCELERATION AT THE SHOCK TRANSITIONS. THE SCOPE AND ACCURACY OF THE CALCULATIONS WE PROPOSE HERE ARE UNPRECEDENTED AND WILL BRING FORTH A QUALITATIVE CHANGE TO THE INTERPRETATION OF SNR OBSERVATIONS. COMPARISONS BETWEEN THESE MODELS AND THE EXCELLENT MULTI-WAVELENGTH DATA SETS NOW IN THE PUBLIC DOMAIN FOR OBJECTS LIKE SN 1987A SN 1996CR CASSIOPEIA A G292.0+1.8 AND 1E 0102.1-7219 WILL ALLOW US TO TEST SPECIFIC SCENARIOS FOR THE EVOLUTION OF CCSN PROGENITORS THEIR PRE-EXPLOSION MASS LOSS AND THE PHYSICS OF THE EXPLOSIONS THEMSELVES. THIS WORK WILL REPRESENT THE FIRST COMPREHENSIVE END-TO-END EFFORT TO CONNECT CCSNE TO THE BULK DYNAMICS AND MULTI-WAVELENGTH EMISSION OF SNRS.