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Supernova 2020wnt: An Atypical Superluminous Supernova with a Hidden Central Engine

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Supernova 2020wnt: An Atypical Superluminous Supernova with a Hidden Central Engine. / Tinyanont, Samaporn; Woosley, Stan E.; Taggart, Kirsty et al.
In: The Astrophysical Journal, Vol. 951, No. 1, 34, 01.07.2023.

Research output: Contribution to Journal/Magazine › Journal article › peer-review

Harvard

Tinyanont, S, Woosley, SE, Taggart, K, Foley, RJ, Yan, L, Lunnan, R, Davis, KW, Kilpatrick, CD, Siebert, MR, Schulze, S, Ashall, C, Chen, T-W, De, K, Dimitriadis, G, Dong, DZ, Fremling, C, Gagliano, A, Jha, SW, Jones, DO, Kasliwal, MM, Miao, H-Y, Pan, Y-C, Perley, DA, Ravi, V, Rojas-Bravo, C, Sfaradi, I, Sollerman, J, Alarcon, V, Angulo, R, Clever, KE, Crawford, P, Couch, C, Dandu, S, Dhara, A, Johnson, J, Lai, Z & Smith, C 2023, 'Supernova 2020wnt: An Atypical Superluminous Supernova with a Hidden Central Engine', The Astrophysical Journal, vol. 951, no. 1, 34. https://doi.org/10.3847/1538-4357/acc6c3

APA

Tinyanont, S., Woosley, S. E., Taggart, K., Foley, R. J., Yan, L., Lunnan, R., Davis, K. W., Kilpatrick, C. D., Siebert, M. R., Schulze, S., Ashall, C., Chen, T.-W., De, K., Dimitriadis, G., Dong, D. Z., Fremling, C., Gagliano, A., Jha, S. W., Jones, D. O., ... Smith, C. (2023). Supernova 2020wnt: An Atypical Superluminous Supernova with a Hidden Central Engine. The Astrophysical Journal, 951(1), Article 34. https://doi.org/10.3847/1538-4357/acc6c3

Vancouver

Tinyanont S, Woosley SE, Taggart K, Foley RJ, Yan L, Lunnan R et al. Supernova 2020wnt: An Atypical Superluminous Supernova with a Hidden Central Engine. The Astrophysical Journal. 2023 Jul 1;951(1):34. doi: 10.3847/1538-4357/acc6c3

Author

Tinyanont, Samaporn ; Woosley, Stan E. ; Taggart, Kirsty et al. / Supernova 2020wnt: An Atypical Superluminous Supernova with a Hidden Central Engine. In: The Astrophysical Journal. 2023 ; Vol. 951, No. 1.

Bibtex

@article{6ff20b7ab66a4309a47143ebbb125be1,
title = "Supernova 2020wnt: An Atypical Superluminous Supernova with a Hidden Central Engine",
abstract = "We present observations of a peculiar hydrogen- and helium-poor stripped-envelope (SE) supernova (SN) 2020wnt, primarily in the optical and near-infrared (near-IR). Its peak absolute bolometric magnitude of −20.9 mag (L bol, peak = (6.8 ± 0.3) × 10 43 erg s −1) and a rise time of 69 days are reminiscent of hydrogen-poor superluminous SNe (SLSNe I), luminous transients potentially powered by spinning-down magnetars. Before the main peak, there is a brief peak lasting <10 days post explosion, likely caused by interaction with circumstellar medium (CSM) ejected ∼years before the SN explosion. The optical spectra near peak lack a hot continuum and O ii absorptions, which are signs of heating from a central engine; they quantitatively resemble those of radioactivity-powered hydrogen/helium-poor Type Ic SESNe. At ∼1 yr after peak, nebular spectra reveal a blue pseudo-continuum and narrow O i recombination lines associated with magnetar heating. Radio observations rule out strong CSM interactions as the dominant energy source at +266 days post peak. Near-IR observations at +200-300 days reveal carbon monoxide and dust formation, which causes a dramatic optical light-curve dip. Pair-instability explosion models predict slow light curve and spectral features incompatible with observations. SN 2020wnt is best explained as a magnetar-powered core-collapse explosion of a 28 M ⊙ pre-SN star. The explosion kinetic energy is significantly larger than the magnetar energy at peak, effectively concealing the magnetar-heated inner ejecta until well after peak. SN 2020wnt falls into a continuum between normal SNe Ic and SLSNe I, and demonstrates that optical spectra at peak alone cannot rule out the presence of a central engine.",
author = "Samaporn Tinyanont and Woosley, {Stan E.} and Kirsty Taggart and Foley, {Ryan J.} and Lin Yan and Ragnhild Lunnan and Davis, {Kyle W.} and Kilpatrick, {Charles D.} and Siebert, {Matthew R.} and Steve Schulze and Chris Ashall and Ting-Wan Chen and Kishalay De and Georgios Dimitriadis and Dong, {Dillon Z.} and Christoffer Fremling and Alexander Gagliano and Jha, {Saurabh W.} and Jones, {David O.} and Kasliwal, {Mansi M.} and Hao-Yu Miao and Yen-Chen Pan and Perley, {Daniel A.} and Vikram Ravi and Cesar Rojas-Bravo and Itai Sfaradi and Jesper Sollerman and Vanessa Alarcon and Rodrigo Angulo and Clever, {Karoli E.} and Payton Crawford and Cirilla Couch and Srujan Dandu and Atirath Dhara and Jessica Johnson and Zhisen Lai and Carli Smith",
year = "2023",
month = jul,
day = "1",
doi = "10.3847/1538-4357/acc6c3",
language = "English",
volume = "951",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing",
number = "1",

}

RIS

TY - JOUR

T1 - Supernova 2020wnt: An Atypical Superluminous Supernova with a Hidden Central Engine

AU - Tinyanont, Samaporn

AU - Woosley, Stan E.

AU - Taggart, Kirsty

AU - Foley, Ryan J.

AU - Yan, Lin

AU - Lunnan, Ragnhild

AU - Davis, Kyle W.

AU - Kilpatrick, Charles D.

AU - Siebert, Matthew R.

AU - Schulze, Steve

AU - Ashall, Chris

AU - Chen, Ting-Wan

AU - De, Kishalay

AU - Dimitriadis, Georgios

AU - Dong, Dillon Z.

AU - Fremling, Christoffer

AU - Gagliano, Alexander

AU - Jha, Saurabh W.

AU - Jones, David O.

AU - Kasliwal, Mansi M.

AU - Miao, Hao-Yu

AU - Pan, Yen-Chen

AU - Perley, Daniel A.

AU - Ravi, Vikram

AU - Rojas-Bravo, Cesar

AU - Sfaradi, Itai

AU - Sollerman, Jesper

AU - Alarcon, Vanessa

AU - Angulo, Rodrigo

AU - Clever, Karoli E.

AU - Crawford, Payton

AU - Couch, Cirilla

AU - Dandu, Srujan

AU - Dhara, Atirath

AU - Johnson, Jessica

AU - Lai, Zhisen

AU - Smith, Carli

PY - 2023/7/1

Y1 - 2023/7/1

N2 - We present observations of a peculiar hydrogen- and helium-poor stripped-envelope (SE) supernova (SN) 2020wnt, primarily in the optical and near-infrared (near-IR). Its peak absolute bolometric magnitude of −20.9 mag (L bol, peak = (6.8 ± 0.3) × 10 43 erg s −1) and a rise time of 69 days are reminiscent of hydrogen-poor superluminous SNe (SLSNe I), luminous transients potentially powered by spinning-down magnetars. Before the main peak, there is a brief peak lasting <10 days post explosion, likely caused by interaction with circumstellar medium (CSM) ejected ∼years before the SN explosion. The optical spectra near peak lack a hot continuum and O ii absorptions, which are signs of heating from a central engine; they quantitatively resemble those of radioactivity-powered hydrogen/helium-poor Type Ic SESNe. At ∼1 yr after peak, nebular spectra reveal a blue pseudo-continuum and narrow O i recombination lines associated with magnetar heating. Radio observations rule out strong CSM interactions as the dominant energy source at +266 days post peak. Near-IR observations at +200-300 days reveal carbon monoxide and dust formation, which causes a dramatic optical light-curve dip. Pair-instability explosion models predict slow light curve and spectral features incompatible with observations. SN 2020wnt is best explained as a magnetar-powered core-collapse explosion of a 28 M ⊙ pre-SN star. The explosion kinetic energy is significantly larger than the magnetar energy at peak, effectively concealing the magnetar-heated inner ejecta until well after peak. SN 2020wnt falls into a continuum between normal SNe Ic and SLSNe I, and demonstrates that optical spectra at peak alone cannot rule out the presence of a central engine.

AB - We present observations of a peculiar hydrogen- and helium-poor stripped-envelope (SE) supernova (SN) 2020wnt, primarily in the optical and near-infrared (near-IR). Its peak absolute bolometric magnitude of −20.9 mag (L bol, peak = (6.8 ± 0.3) × 10 43 erg s −1) and a rise time of 69 days are reminiscent of hydrogen-poor superluminous SNe (SLSNe I), luminous transients potentially powered by spinning-down magnetars. Before the main peak, there is a brief peak lasting <10 days post explosion, likely caused by interaction with circumstellar medium (CSM) ejected ∼years before the SN explosion. The optical spectra near peak lack a hot continuum and O ii absorptions, which are signs of heating from a central engine; they quantitatively resemble those of radioactivity-powered hydrogen/helium-poor Type Ic SESNe. At ∼1 yr after peak, nebular spectra reveal a blue pseudo-continuum and narrow O i recombination lines associated with magnetar heating. Radio observations rule out strong CSM interactions as the dominant energy source at +266 days post peak. Near-IR observations at +200-300 days reveal carbon monoxide and dust formation, which causes a dramatic optical light-curve dip. Pair-instability explosion models predict slow light curve and spectral features incompatible with observations. SN 2020wnt is best explained as a magnetar-powered core-collapse explosion of a 28 M ⊙ pre-SN star. The explosion kinetic energy is significantly larger than the magnetar energy at peak, effectively concealing the magnetar-heated inner ejecta until well after peak. SN 2020wnt falls into a continuum between normal SNe Ic and SLSNe I, and demonstrates that optical spectra at peak alone cannot rule out the presence of a central engine.

U2 - 10.3847/1538-4357/acc6c3

DO - 10.3847/1538-4357/acc6c3

M3 - Journal article

VL - 951

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 34

ER -