Schulze, S, Fransson, C, Kozyreva, A, Chen, TW, Yaron, O, Jerkstrand, A, Gal-Yam, A, Sollerman, J, Yan, L, Kangas, T, Leloudas, G, Omand, CMB, Smartt, SJ, Yang, Y, Nicholl, M, Sarin, N, Yao, Y, Brink, TG, Sharon, A, Rossi, A et al, Chen, P, Chen, Z, Cikota, A, De, K, Drake, AJ, Filippenko, AV, Fremling, C, Fréour, L, Fynbo, JPU, Ho, AYQ, Inserra, C, Irani, I, Kuncarayakti, H, Lunnan, R, Mazzali, P, Ofek, EO, Palazzi, E, Perley, DA, Pursiainen, M, Rothberg, B, Shingles, LJ, Smith, K, Taggart, K, Tartaglia, L, Zheng, WK, Anderson, JP, Cassara, L, Christensen, E, Djorgovski, SG, Galbany, L, Gkini, A, Graham, MJ, Gromadzki, M, Groom, SL, Hiramatsu, D, Howell, DA, Kasliwal, MM, McCully, C, Müller-Bravo, TE, Paiano, S, Paraskeva, E, Pessi, PJ, Polishook, D, Rau, A, Rigault, M and Rusholme, B (2024) 1100 days in the life of the supernova 2018ibb The best pair-instability supernova candidate, to date. Astronomy & Astrophysics, 683. ISSN 0004-6361

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Abstract

Stars with zero-age main sequence masses between 140 and 260 M are thought to explode as pair-instability supernovae (PISNe). During their thermonuclear runaway, PISNe can produce up to several tens of solar masses of radioactive nickel, resulting in luminous transients similar to some superluminous supernovae (SLSNe). Yet, no unambiguous PISN has been discovered so far. SN 2018ibb is a hydrogen-poor SLSN at z = 0.166 that evolves extremely slowly compared to the hundreds of known SLSNe. Between mid 2018 and early 2022, we monitored its photometric and spectroscopic evolution from the UV to the near-infrared (NIR) with 2–10 m class telescopes. SN 2018ibb radiated >3 × 1051 erg during its evolution, and its bolometric light curve reached >2 × 1044 erg s−1 at its peak. The long-lasting rise of >93 rest-frame days implies a long diffusion time, which requires a very high total ejected mass. The PISN mechanism naturally provides both the energy source (56Ni) and the long diffusion time. Theoretical models of PISNe make clear predictions as to their photometric and spectroscopic properties. SN 2018ibb complies with most tests on the light curves, nebular spectra and host galaxy, and potentially all tests with the interpretation we propose. Both the light curve and the spectra require 25–44 M of freshly nucleosynthesised 56Ni, pointing to the explosion of a metal-poor star with a helium core mass of 120–130 M at the time of death. This interpretation is also supported by the tentative detection of [Co ii] λ 1.025 µm, which has never been observed in any other PISN candidate or SLSN before. We observe a significant excess in the blue part of the optical spectrum during the nebular phase, which is in tension with predictions of existing PISN models. However, we have compelling observational evidence for an eruptive mass-loss episode of the progenitor of SN 2018ibb shortly before the explosion, and our dataset reveals that the interaction of the SN ejecta with this oxygen-rich circumstellar material contributed to the observed emission. That may explain this specific discrepancy with PISN models. Powering by a central engine, such as a magnetar or a black hole, can be excluded with high confidence. This makes SN 2018ibb by far the best candidate for being a PISN, to date.

Item Type:	Article
Uncontrolled Keywords:	0201 Astronomical and Space Sciences; Astronomy & Astrophysics
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Divisions:	Astrophysics Research Institute
Publisher:	EDP Sciences
SWORD Depositor:	A Symplectic
Date Deposited:	20 Jun 2024 11:21
Last Modified:	20 Jun 2024 11:30
DOI or ID number:	10.1051/0004-6361/202346855
URI:	https://researchonline.ljmu.ac.uk/id/eprint/23609

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