Facial reconstruction

Search LJMU Research Online

Browse Repository | Browse E-Theses

Dramatic rebrightening of the type-changing stripped-envelope supernova SN 2023aew

Sharma, Y, Sollerman, J, Kulkarni, SR, Moriya, TJ, Schulze, S, Barmentloo, S, Fausnaugh, M, Gal-Yam, A, Jerkstrand, A, Ahumada, T, Bellm, EC, Das, KK, Drake, A, Fremling, C, Hale, D, Hall, S, Hinds, KR, Laz, TJD, Karambelkar, V, Kasliwal, MM , Masci, FJ, Miller, AA, Nir, G, Perley, DA, Purdum, JN, Qin, Y-J, Rehemtulla, N, Rich, RM, Riddle, RL, Rodriguez, AC, Rose, S, Somalwar, J, Wise, JL, Wold, A, Yan, L and Yao, Y (2024) Dramatic rebrightening of the type-changing stripped-envelope supernova SN 2023aew. The Astrophysical Journal, 966 (2). ISSN 0004-637X

Dramatic Rebrightening of the Type-changing Stripped-envelope Supernova SN 2023aew.pdf - Published Version
Available under License Creative Commons Attribution.

Download (12MB) | Preview


Multipeaked supernovae with precursors, dramatic light-curve rebrightenings, and spectral transformation are rare, but are being discovered in increasing numbers by modern night-sky transient surveys like the Zwicky Transient Facility. Here, we present the observations and analysis of SN 2023aew, which showed a dramatic increase in brightness following an initial luminous (−17.4 mag) and long (∼100 days) unusual first peak (possibly precursor). SN 2023aew was classified as a Type IIb supernova during the first peak but changed its type to resemble a stripped-envelope supernova (SESN) after the marked rebrightening. We present comparisons of SN 2023aew's spectral evolution with SESN subtypes and argue that it is similar to SNe Ibc during its main peak. P-Cygni Balmer lines are present during the first peak, but vanish during the second peak's photospheric phase, before Hα resurfaces again during the nebular phase. The nebular lines ([O i], [Ca ii], Mg i], Hα) exhibit a double-peaked structure that hints toward a clumpy or nonspherical ejecta. We analyze the second peak in the light curve of SN 2023aew and find it to be broader than that of normal SESNe as well as requiring a very high 56Ni mass to power the peak luminosity. We discuss the possible origins of SN 2023aew including an eruption scenario where a part of the envelope is ejected during the first peak and also powers the second peak of the light curve through interaction of the SN with the circumstellar medium.

Item Type: Article
Uncontrolled Keywords: astro-ph.HE; astro-ph.HE
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: American Astronomical Society
Related URLs:
SWORD Depositor: A Symplectic
Date Deposited: 16 May 2024 10:06
Last Modified: 16 May 2024 10:06
DOI or ID number: 10.3847/1538-4357/ad3758
URI: https://researchonline.ljmu.ac.uk/id/eprint/23272
View Item View Item