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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/29326
Title: SN 2016coi (ASASSN-16fp): An Energetic H-stripped Core-collapse Supernova from a Massive Stellar Progenitor with Large Mass Loss
Authors: Terreran, G.
Margutti, R.
Bersier, D.
Brimacombe, J.
Caprioli, D.
Challis, P.
Chornock, R.
Coppejans, D. L.
Dong, Subo
Guidorzi, C.
Hurley, K.
Kirshner, R.
Migliori, G.
Milisavljevic, D.
Palmer, D. M.
Prieto, J. L.
TOMASELLA, Lina 
Marchant, P.
Pastorello, A.
Shappee, B. J.
Stanek, K. Z.
Stritzinger, M. D.
Benetti, S.
Chen, Ping
DeMarchi, L.
ELIAS DE LA ROSA, NANCY DEL CARMEN 
Gall, C.
Harmanen, J.
Mattila, S.
Issue Date: 2019
Journal: THE ASTROPHYSICAL JOURNAL 
Number: 883
Issue: 2
First Page: 147
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 <SUB>ej</SUB> ∼ 4-7 M <SUB>☉</SUB>, E <SUB>k</SUB> ∼ (7-8) × 10<SUP>51</SUP> 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 <SUB>X</SUB> > 10<SUP>39</SUP> erg s<SUP>-1</SUP> in the first ∼100 days post explosion) and radio emission (L <SUB>8.5 GHz</SUB> ∼ 7 × 10<SUP>27</SUP> erg s<SUP>-1</SUP> Hz<SUP>-1</SUP> 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}<SUP>-4</SUP> {M}<SUB>☉ </SUB> {yr}}<SUP>-1</SUP> and a sub-relativistic shock velocity v <SUB>sh</SUB> ∼ 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 <SUB> γ </SUB> > 2 × 10<SUP>46</SUP> 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.
URI: http://hdl.handle.net/20.500.12386/29326
URL: https://iopscience.iop.org/article/10.3847/1538-4357/ab3e37
ISSN: 0004-637X
DOI: 10.3847/1538-4357/ab3e37
Bibcode ADS: 2019ApJ...883..147T
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

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