Twin peaks: SN 2021uvy and SN 2022hgk in the landscape of double-peaked stripped envelope supernovae

TL;DR

This paper explores the diversity and underlying powering mechanisms of double-peaked stripped-envelope supernovae by analyzing two new cases and comparing them with a broader sample, revealing correlations and potential classification criteria.

Contribution

It introduces two new double-peaked SESNe, SN 2021uvy and SN 2022hgk, and provides a comprehensive analysis of their properties within the context of existing supernova data, highlighting the variety of powering mechanisms.

Findings

A correlation between the first and second peak magnitudes (p-value~0.025).

Multiple powering mechanisms are needed to explain the diversity in the sample.

A phase-space map (duration vs magnitude difference) to distinguish powering mechanisms.

Abstract

In recent years, a class of stripped-envelope supernovae (SESNe) showing two distinct light-curve peaks has emerged, where the first peak cannot be attributed to shock cooling emission. Such peculiar SNe are often studied individually, explained by a combination of powering mechanisms, but are rarely discussed broadly as a group. In this paper, we attempt to form a picture of the landscape of double-peaked SESNe and their powering mechanisms by adding two more objects -- SN 2021uvy and SN 2022hgk. SN 2021uvy is a broad, luminous SN Ib with an unusually long first peak rise and constant color evolution with rising photospheric temperature during the second peak. Though its first peak resembles SN 2019stc, their second peaks differ, making SN 2021uvy unique. SN 2022hgk shows photometric similarity to SN 2019cad and spectroscopic similarity to SN 2005bf, both proposed to be powered by a double-nickel distribution in their ejecta. We analyze their light curves and colors, compare them with a sample of double-peaked SESNe from the ZTF archive, and analyze the light curve parameters of the sample. We observe a correlation (p-value~0.025) between the peak absolute magnitudes of the first and second peaks. No single definitive powering mechanism applies to the whole sample, as it shows variety in the photometric and spectroscopic properties. However, sub-groups of similarity exist that can be explained by mechanisms like the double-nickel distribution, magnetar central engine, interaction, and fallback accretion. We also map out the duration between the peaks ($\Delta t^{21}$) vs the difference between peak absolute magnitudes ($\Delta M^{21}$) as a phase-space that could potentially delineate the most promising powering mechanisms for the double-peaked SESNe.