The Superluminous Type IIn Supernova ASASSN-15ua: Part of a continuum in extreme precursor mass loss

We present a series of ground-based photometry and spectroscopy of the superluminous Type IIn supernova (SN) ASASSN-15ua, which shows evidence for strong interaction with pre-existing dense circumstellar material (CSM). Our observations constrain the speed, mass-loss rate, and extent of the progenitor wind shortly before explosion. A narrow P Cygni absorption component reveals a progenitor wind speed of \(\sim\)100 km s\(^{-1}\). As observed in previous SNe IIn, the intermediate-width H\(\alpha\) emission became more asymmetric and blueshifted over time, suggesting either asymmetric CSM, an asymmetric explosion, or increasing selective extinction from dust within the post-shock shell or SN ejecta. Based on the CSM radius and speed, we find that the progenitor suffered extreme eruptive mass loss with a rate of 0.1-1 M\(_\odot\) yr\(^{-1}\) during the \(\sim\)12 years immediately before the death of the star that imparted \(\sim\) 10\(^{48}\) erg of kinetic energy to the CSM. Integrating its \(V\)-band light curve over the first 170 days after discovery, we find that ASASSN-15ua radiated at least 3\(\times\)10\(^{50}\) erg in visual light alone, giving a lower limit to the total radiated energy that may have approached 10\(^{51}\) erg. ASASSN-15ua exhibits many similarities to two well-studied superluminous SNe IIn: SN 2006tf and SN 2010jl. Based on a detailed comparison of these three, we find that ASASSN-15ua falls in between these two events in a wide variety of observed properties and derived physical parameters, illustrating a continuum of behavior across superluminous SNe IIn.