Multiwavelength Signals from Pulsar-Driven Supernovae

The pulsar-driven supernova model, where the spin-down energy of a ~ms rotating highly magnetized neutron star powers the luminosity and/or dynamics of the supernova, can be used to explain a number of transients, most notably Type-I Super-Luminous Supernovae (SLSNe-I).  In this model, the energy from the pulsar is injected into the ejecta through broadband emission from the pulsar wind nebula (PWN).  There are several models which can explain SLSNe-I light curves, so quasi-thermal optical supernova emission can not differentiate between different central supernova engines, but this non-thermal PWN emission is unique to the pulsar engine.   We calculated the expected radio and millimetre PWN emission from several SLSNe-I, and then did follow-up observations to test these predictions.  We also investigated the effect of PWNe on dust formation and calculated the emission from grains heated by the PWN.