Details

Autor(en) / Beteiligte

• Sharma, Yashvi
• Sollerman, Jesper
• Kulkarni, Shrinivas R.
• Moriya, Takashi J.
• Schulze, Steve
• Barmentloo, Stan
• Fausnaugh, Michael
• Gal-Yam, Avishay
• Jerkstrand, Anders
• Ahumada, Tomás
• Bellm, Eric C.
• Das, Kaustav K.
• Drake, Andrew
• Fremling, Christoffer
• Hale, David
• Hall, Saarah
• Hinds, K. R.
• du Laz, Theophile Jegou
• Karambelkar, Viraj
• Kasliwal, Mansi M.
• Masci, Frank J.
• Miller, Adam A.
• Nir, Guy
• Perley, Daniel A.
• Purdum, Josiah N.
• Qin, Yu-Jing
• Rehemtulla, Nabeel
• Rich, R. Michael
• Riddle, Reed L.
• Rodriguez, Antonio C.
• Rose, Sam
• Somalwar, Jean
• Wise, Jacob L.
• Wold, Avery
• Yan, Lin
• Yao, Yuhan

Titel

Dramatic Rebrightening of the Type-changing Stripped-envelope Supernova SN 2023aew

Ist Teil von

• The Astrophysical journal, 2024-05, Vol.966 (2), p.199

Ort / Verlag

Philadelphia: IOP Publishing

Erscheinungsjahr

2024

Link zum Volltext

Quelle

Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals

Beschreibungen/Notizen

• Abstract 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 H α resurfaces again during the nebular phase. The nebular lines ([O i ], [Ca ii ], Mg i ], H α ) 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 56 Ni 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.