SN2016coi (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. Shappee; K. Z. Stanek; M. D. Stritzinger; S. Benetti; Ping Chen; L. Demarchi; N. Elias-Rosa; C. Gall; J. Harmanen; S. Mattila

doi:10.3847/1538-4357/ab3e37

SN2016coi (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, S. Mattila

DARK

9 Citationer (Scopus)

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 _o, 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 M ∼ (1-2) × 10^-4M_⊙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.

Originalsprog	Engelsk
Artikelnummer	147
Tidsskrift	Astrophysical Journal
Vol/bind	883
Udgave nummer	2
Antal sider	29
ISSN	0004-637X
DOI	https://doi.org/10.3847/1538-4357/ab3e37
Status	Udgivet - 1 okt. 2019

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10.3847/1538-4357/ab3e37

https://iopscience.iop.org/article/10.3847/1538-4357/ab3e37/pdf

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Terreran, G., Margutti, R., Bersier, D., Brimacombe, J., Caprioli, D., Challis, P., Chornock, R., Coppejans, D. L., Dong, S., Guidorzi, C., Hurley, K., Kirshner, R., Migliori, G., Milisavljevic, D., Palmer, D. M., Prieto, J. L., Tomasella, L., Marchant, P., Pastorello, A., ... 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), [147]. https://doi.org/10.3847/1538-4357/ab3e37

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 & Mattila, S 2019, 'SN2016coi (ASASSN-16fp): An Energetic H-stripped Core-collapse Supernova from a Massive Stellar Progenitor with Large Mass Loss', Astrophysical Journal, bind 883, nr. 2, 147. https://doi.org/10.3847/1538-4357/ab3e37

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title = "SN2016coi (ASASSN-16fp): An Energetic H-stripped Core-collapse Supernova from a Massive Stellar Progenitor with Large Mass Loss",

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 o, 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 M ∼ (1-2) × 10-4M⊙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.",

keywords = "supernovae: individual (SN 2016coi, ASASSN-16fp)",

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

year = "2019",

month = oct,

day = "1",

doi = "10.3847/1538-4357/ab3e37",

language = "English",

volume = "883",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "Institute of Physics Publishing, Inc",

number = "2",

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TY - JOUR

T1 - SN2016coi (ASASSN-16fp)

T2 - An Energetic H-stripped Core-collapse Supernova from a Massive Stellar Progenitor with Large Mass Loss

AU - Terreran, G.

AU - Margutti, R.

AU - Bersier, D.

AU - Brimacombe, J.

AU - Caprioli, D.

AU - Challis, P.

AU - Chornock, R.

AU - Coppejans, D. L.

AU - Dong, Subo

AU - Guidorzi, C.

AU - Hurley, K.

AU - Kirshner, R.

AU - Migliori, G.

AU - Milisavljevic, D.

AU - Palmer, D. M.

AU - Prieto, J. L.

AU - Tomasella, L.

AU - Marchant, P.

AU - Pastorello, A.

AU - Shappee, B. J.

AU - Stanek, K. Z.

AU - Stritzinger, M. D.

AU - Benetti, S.

AU - Chen, Ping

AU - Demarchi, L.

AU - Elias-Rosa, N.

AU - Gall, C.

AU - Harmanen, J.

AU - Mattila, S.

PY - 2019/10/1

Y1 - 2019/10/1

N2 - 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 o, 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 M ∼ (1-2) × 10-4M⊙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.

AB - 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 o, 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 M ∼ (1-2) × 10-4M⊙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.

KW - supernovae: individual (SN 2016coi, ASASSN-16fp)

U2 - 10.3847/1538-4357/ab3e37

DO - 10.3847/1538-4357/ab3e37

M3 - Journal article

SN - 0004-637X

VL - 883

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 147

ER -

SN2016coi (ASASSN-16fp): An Energetic H-stripped Core-collapse Supernova from a Massive Stellar Progenitor with Large Mass Loss

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