SN 2016coi (ASASSN-16fp): An energetic h-stripped core-collapse supernova from a massive stellar progenitor with large mass loss

G. Terreran, R. Margutti, D. Bersier, J. Brimacombe, D. Caprioli, P. Challis, R. Chornock, D. L. Coppejans, Subo Dong, C. Guidorzi, K. Hurley, R. Kirshner, G. Migliori, D. Milisavljevic, D. M. Palmer, J. L. Prieto, L. Tomasella, P. Marchant, A. Pastorello, B. J. ShappeeK. Z. Stanek, M. D. Stritzinger, S. Benetti, Ping Chen, L. Demarchi, N. Elias-Rosa, C. Gall, J. Harmanen, And S. Mattila

Research output: Contribution to journalArticlepeer-review

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 SN ejecta, which we interpret to be caused by a larger mixing of Ni into the outer ejecta layers. From the modeling of the broad bolometric light curve we derive a large ejecta mass to kinetic energy ratio (Mej ∼ 4 − 7 M☉, Ek ∼ 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 (LX > 1039 erg s−1 in the first ∼ 100 days post explosion) and radio emission (L8.5 GHz ∼ 7 × 1027 erg s−1Hz−1 at peak). These values are in line with those of relativistic SNe (2009bb, 2012ap). However, for SN 2016coi we infer substantial

Original languageEnglish (US)
JournalUnknown Journal
StatePublished - May 6 2019

ASJC Scopus subject areas

  • General

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