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Terreran, G, Margutti, R, Bersier, D, Brimacombe, J, Caprioli, D, Challis, P, Chornock, R, Coppejans, DL, Dong, S, Guidorzi, C, Hurley, K, Kirshner, R, Migliori, G, Milisavljevic, D, Palmer, DM, Prieto, JL, Tomasella, L, Marchant, P, Pastorello, A, Shappee, BJ , Stanek, KZ, Stritzinger, MD, Benetti, S, Chen, P, Demarchi, L, Elias-Rosa, N, Gall, C, Harmanen, J and Mattila, S (2019) SN2016coi (ASASSN-16fp): An Energetic H-stripped Core-collapse Supernova from a Massive Stellar Progenitor with Large Mass Loss. Astrophysical Journal, 883 (2). ISSN 0004-637X
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Abstract
We present comprehensive observations and analysis of the energetic H-stripped SN 2016coi (a.k.a. ASASSN-16fp), spanning the γ-ray through optical and radio wavelengths, acquired within the first hours to ~420 days post explosion. Our observational campaign confirms the identification of He in the supernova (SN) ejecta, which we interpret to be caused by a larger mixing of Ni into the outer ejecta layers. By modeling the broad bolometric light curve, we derive a large ejecta-mass-to-kinetic-energy ratio (M ej ~ 4–7 M ⊙, E k ~ (7–8) × 1051 erg). The small [Ca ii] λλ7291,7324 to [O i] λλ6300,6364 ratio (~0.2) observed in our late-time optical spectra is suggestive of a large progenitor core mass at the time of collapse. We find that SN 2016coi is a luminous source of X-rays (L X > 1039 erg s−1 in the first ~100 days post explosion) and radio emission (L 8.5 GHz ~ 7 × 1027 erg s−1 Hz−1 at peak). These values are in line with those of relativistic SNe (2009bb, 2012ap). However, for SN 2016coi, we infer substantial pre-explosion progenitor mass loss with a rate $\dot{M}$ ~ (1–2) × ${10}^{-4}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}$ and a sub-relativistic shock velocity v sh ~ 0.15c, which is in stark contrast with relativistic SNe and similar to normal SNe. Finally, we find no evidence for a SN-associated shock breakout γ-ray pulse with energy E γ > 2 × 1046 erg. While we cannot exclude the presence of a companion in a binary system, taken together, our findings are consistent with a massive single-star progenitor that experienced large mass loss in the years leading up to core collapse, but was unable to achieve complete stripping of its outer layers before explosion.
| Item Type: | Article |
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| Uncontrolled Keywords: | Science & Technology; Physical Sciences; Astronomy & Astrophysics; supernovae: individual (SN 2016coi, ASASSN-16fp); X-RAY OBSERVATIONS; DIGITAL SKY SURVEY; RADIO-EMISSION; LIGHT CURVES; PRESUPERNOVA EVOLUTION; PARTICLE-ACCELERATION; NEBULAR SPECTRA; IB/C SUPERNOVAE; LINE-PROFILES; IBC SUPERNOVA; Science & Technology; Physical Sciences; Astronomy & Astrophysics; supernovae: individual (SN 2016coi, ASASSN-16fp); X-RAY OBSERVATIONS; DIGITAL SKY SURVEY; RADIO-EMISSION; LIGHT CURVES; PRESUPERNOVA EVOLUTION; PARTICLE-ACCELERATION; NEBULAR SPECTRA; IB/C SUPERNOVAE; LINE-PROFILES; IBC SUPERNOVA; astro-ph.HE; astro-ph.HE; 0201 Astronomical and Space Sciences; 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics; 0306 Physical Chemistry (incl. Structural); Astronomy & Astrophysics |
| 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: | 05 May 2022 11:53 |
| Last Modified: | 05 May 2022 12:00 |
| DOI or ID number: | 10.3847/1538-4357/ab3e37 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/16759 |
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