Description
One of the most promising models to explain SLSNe is the magnetar model. In this scenario, the spin-down energy from a rapidly-rotating neutron star is injected into the supernova ejecta via a pulsar wind nebula (PWN). The PWN both accelerates the ejecta and produces broadband emission that is absorbed and thermalized in the ejecta. Since the light curves of magnetar-driven SLSNe are indistinguishable from those produced by other scenarios, observations at late times are key to testing the magnetar model. I will overview some of the proposed late-time signals, including radio emission from the PWN and infrared/optical spectral lines from the photoionized ejecta, with a focus on what can be detectable with new and upcoming instruments such as JWST and ngVLA.
