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The Type Icn SN 2021csp: Implications for the Origins of the Fastest Supernovae and the Fates of Wolf-Rayet Stars

Perley, DA, Sollerman, J, Schulze, S, Yao, Y, Fremling, C, Gal-Yam, A, Ho, AYQ, Yang, Y, Kool, EC, Irani, I, Yan, L, Andreoni, I, Baade, D, Bellm, EC, Brink, TG, Chen, T-W, Cikota, A, Coughlin, MW, Dahiwale, A, Dekany, R , Duev, DA, Filippenko, A, Hoeflich, P, Kasliwal, MM, Kulkarni, SR, Lunnan, R, Masci, FJ, Maund, JR, Medford, MS, Riddle, R, Rosnet, P, Shupe, DL, Strotjohann, NL, Tzanidakis, A and Zheng, W (2022) The Type Icn SN 2021csp: Implications for the Origins of the Fastest Supernovae and the Fates of Wolf-Rayet Stars. Astrophysical Journal, 927 (2). ISSN 0004-637X

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Open Access URL: https://iopscience.iop.org/article/10.3847/1538-43... (Published version)


We present observations of SN 2021csp, the second example of a newly identified type of supernova (SN) hallmarked by strong, narrow, P Cygni carbon features at early times (Type Icn). The SN appears as a fast and luminous blue transient at early times, reaching a peak absolute magnitude of -20 within 3 days due to strong interaction between fast SN ejecta (v ≈ 30,000 km s-1) and a massive, dense, fast-moving C/O wind shed by the WC-like progenitor months before explosion. The narrow-line features disappear from the spectrum 10-20 days after explosion and are replaced by a blue continuum dominated by broad Fe features, reminiscent of Type Ibn and IIn supernovae and indicative of weaker interaction with more extended H/He-poor material. The transient then abruptly fades ∼60 days post-explosion when interaction ceases. Deep limits at later phases suggest minimal heavy-element nucleosynthesis, a low ejecta mass, or both, and imply an origin distinct from that of classical Type Ic SNe. We place SN 2021csp in context with other fast-evolving interacting transients, and discuss various progenitor scenarios: an ultrastripped progenitor star, a pulsational pair-instability eruption, or a jet-driven fallback SN from a Wolf-Rayet (W-R) star. The fallback scenario would naturally explain the similarity between these events and radio-loud fast transients, and suggests a picture in which most stars massive enough to undergo a W-R phase collapse directly to black holes at the end of their lives.

Item Type: Article
Uncontrolled Keywords: Science & Technology; Physical Sciences; Astronomy & Astrophysics; RICH CIRCUMSTELLAR MEDIUM; STRIPPED-ENVELOPE SUPERNOVAE; RAPIDLY RISING TRANSIENTS; DELAY-TIME DISTRIBUTION; LUMINOUS X-RAY; CORE-COLLAPSE; MASSIVE STARS; LIGHT CURVES; SUPERLUMINOUS SUPERNOVAE; PHYSICAL-PROPERTIES; Astronomy & Astrophysics; 0201 Astronomical and Space Sciences; 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics; 0306 Physical Chemistry (incl. Structural)
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: American Astronomical Society; IOP Publishing
SWORD Depositor: A Symplectic
Date Deposited: 30 Jun 2022 09:56
Last Modified: 30 Jun 2022 10:00
DOI or ID number: 10.3847/1538-4357/ac478e
URI: https://researchonline.ljmu.ac.uk/id/eprint/17180
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