Probing the progenitor origins of core-collapse supernova remnants using their broadband non-thermal emission and hydrodynamic models

While the art of linking supernova remnants (SNRs) to their progenitor origins has mostly been basing on their observed thermal X-ray emission and the elemental abundance patterns deduced in their ejecta, the connection between the nature of the exploded stars and the non-thermal emission seen in their remnants hundreds or thousands of years post-explosion has not been explored in depth so far. We use hydrodynamic simulations to model the long-term evolution of SNR non-thermal emission and search for their possible correlations with the explosion properties and circumstellar environments associated with specific types of core-collapse supernovae (CCSNe). Highly characteristic relations between the broadband non-thermal light-curve/spectral evolution and types of the originating CCSNe are discovered. In particular, we found that remnants of Type II SNe and stripped envelope SNe such as Type Ib/c show distinctive time evolution in their radio and gamma-ray luminosities, with the former bright in the early phase but experiencing a "dark age" from about 1000 yrs old for several thousands years, whereas the latter exhibits the exactly opposite behavior. Furthermore, by combining the spectral evolution results from both normal Type II and Type Ib/c progenitors, we have succeeded to propose a model which can explain the variety of gamma-ray spectra seen in young, Sedov phase and middle-aged SNRs by Fermi LAT and air Cherenkov telescopes. The implications of these findings on our understanding of the SNR populations will also be discussed.