Fading Echoes of Interaction: Probing Centuries of Mass-Loss in Four Old Type IIn Supernovae

Abstract: Supernovae characterized by enduring narrow optical hydrogen emission lines (SNe IIn) are believed to result primarily from the core-collapse of massive stars undergoing sustained interaction with a dense circumstellar medium (CSM). While the properties of SN IIn progenitors have relatively few direct constraints, the ongoing ejecta-CSM interaction provides unique information about late-stage stellar mass-loss preceding core-collapse. We present late-time X-ray and radio observations of four $\geq$3000 day-old SNe IIn: SN 2013L, SN 2014ab, SN 2015da, and KISS15s. The radio and X-ray emission from KISS15s indicate a mass-loss rate of $$\rm{\dot M\sim4\times 10<sup>{-3}~{M_{\odot}\,yr<sup>{-1}}}$$ at $\sim$450 years pre-supernova -- 2 orders of magnitude below earlier optical estimates (which probed the mass-loss immediately preceding the supernova). We find hints of a spectral inversion in the radio SED of KISS15s; a possible signature of a secondary shock due to a binary system or the emergence of a pulsar wind. For SN 2013L, we obtain a mass-loss rate of $$\rm{\dot M\sim2 \times 10<sup>{-3}~\rm{M_{\odot}\,yr<sup>{-1}}}$$ at $\sim$400 years pre-explosion based on the X-ray detection. For SN 2014ab and SN 2015da, we find a upper limits on the mass-loss rates of $\rm{\dot M&lt;2\times10<sup>{-3}~M_{\odot}\,yr<sup>{-1}}$ explosion at $\sim$ 250 and 300 years pre-explosion, respectively. All four objects display mass-loss rates lower than estimates from earlier optical analyses by at least 1-3 orders of magnitude, necessitating a rapidly evolving progenitor process over the last centuries pre-explosion. Our analysis reveals how X-ray and radio observations can elucidate progenitor evolution when these objects have faded at optical wavelengths.