Multiple Peaks and a Long Precursor in the Type IIn Supernova 2021qqp: An Energetic Explosion in a Complex Circumstellar Environment

Abstract

We present optical photometry and spectroscopy of the Type IIn supernova (SN) 2021qqp. Its unusual light curve is marked by a long precursor for $\approx 300$ days, a rapid increase in brightness for $\approx 60$ days, and then a sharp increase of $\approx 1.6$ mag in only a few days to a first peak of $M_r\approx -19.5$ mag. The light curve then declines rapidly until it re-brightens to a second distinct peak of $M_r\approx -17.3$ mag centered at $\approx 335$ days after the first peak. The spectra are dominated by Balmer lines with a complex morphology, including a narrow component with a width of $\approx 1300$ km s${}^{-1}$ (first peak) and $\approx 2500$ km s${}^{-1}$ (second peak) that we associate with the circumstellar medium (CSM) and a P Cygni component with an absorption velocity of $\approx 8500$ km s${}^{-1}$ (first peak) and $\approx 5600$ km s${}^{-1}$ (second peak) that we associate with the SN-CSM interaction shell. Using the luminosity and velocity evolution, we construct a flexible analytical model, finding two significant mass-loss episodes with peak mass loss rates of $\approx 10$ and $\approx 5M_{\odot }$ yr${}^{-1}$ about $0.8$ and $2$ yr before explosion, respectively, with a total CSM mass of $\approx 2-4M_{\odot }$. We show that the most recent mass-loss episode could explain the precursor for the year preceding the explosion. The SN ejecta mass is constrained to be $\approx 5-30M_{\odot }$ for an explosion energy of $\approx (3-10)\times 10^{51}$ erg. We discuss eruptive massive stars (luminous blue variable, pulsational pair instability) and an extreme stellar merger with a compact object as possible progenitor channels.

Updated to match the published article in ApJ, 2024 March 29

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