SN 2020wnt: a slow-evolving carbon-rich superluminous supernova with no O II lines and a bumpy light curve

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SN 2020wnt : a slow-evolving carbon-rich superluminous supernova with no O II lines and a bumpy light curve. / Gutierrez, C. P.; Pastorello, A.; Bersten, M.; Benetti, S.; Orellana, M.; Fiore, A.; Karamehmetoglu, E.; Kravtsov, T.; Reguitti, A.; Reynolds, T. M.; Valerin, G.; Mazzali, P.; Sullivan, M.; Cai, Y-Z; Elias-Rosa, N.; Fraser, M.; Hsiao, E. Y.; Kankare, E.; Kotak, R.; Kuncarayakti, H.; Li, Z.; Mattila, S.; Mo, J.; Moran, S.; Ochner, P.; Shahbandeh, M.; Tomasella, L.; Wang, X.; Yan, S.; Zhang, J.; Zhang, T.; Stritzinger, M. D.

In: Monthly Notices of the Royal Astronomical Society, Vol. 517, No. 2, 17.10.2022, p. 2056-2075.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Gutierrez, CP, Pastorello, A, Bersten, M, Benetti, S, Orellana, M, Fiore, A, Karamehmetoglu, E, Kravtsov, T, Reguitti, A, Reynolds, TM, Valerin, G, Mazzali, P, Sullivan, M, Cai, Y-Z, Elias-Rosa, N, Fraser, M, Hsiao, EY, Kankare, E, Kotak, R, Kuncarayakti, H, Li, Z, Mattila, S, Mo, J, Moran, S, Ochner, P, Shahbandeh, M, Tomasella, L, Wang, X, Yan, S, Zhang, J, Zhang, T & Stritzinger, MD 2022, 'SN 2020wnt: a slow-evolving carbon-rich superluminous supernova with no O II lines and a bumpy light curve', Monthly Notices of the Royal Astronomical Society, vol. 517, no. 2, pp. 2056-2075. https://doi.org/10.1093/mnras/stac2747

APA

Gutierrez, C. P., Pastorello, A., Bersten, M., Benetti, S., Orellana, M., Fiore, A., Karamehmetoglu, E., Kravtsov, T., Reguitti, A., Reynolds, T. M., Valerin, G., Mazzali, P., Sullivan, M., Cai, Y-Z., Elias-Rosa, N., Fraser, M., Hsiao, E. Y., Kankare, E., Kotak, R., ... Stritzinger, M. D. (2022). SN 2020wnt: a slow-evolving carbon-rich superluminous supernova with no O II lines and a bumpy light curve. Monthly Notices of the Royal Astronomical Society, 517(2), 2056-2075. https://doi.org/10.1093/mnras/stac2747

Vancouver

Gutierrez CP, Pastorello A, Bersten M, Benetti S, Orellana M, Fiore A et al. SN 2020wnt: a slow-evolving carbon-rich superluminous supernova with no O II lines and a bumpy light curve. Monthly Notices of the Royal Astronomical Society. 2022 Oct 17;517(2):2056-2075. https://doi.org/10.1093/mnras/stac2747

Author

Gutierrez, C. P. ; Pastorello, A. ; Bersten, M. ; Benetti, S. ; Orellana, M. ; Fiore, A. ; Karamehmetoglu, E. ; Kravtsov, T. ; Reguitti, A. ; Reynolds, T. M. ; Valerin, G. ; Mazzali, P. ; Sullivan, M. ; Cai, Y-Z ; Elias-Rosa, N. ; Fraser, M. ; Hsiao, E. Y. ; Kankare, E. ; Kotak, R. ; Kuncarayakti, H. ; Li, Z. ; Mattila, S. ; Mo, J. ; Moran, S. ; Ochner, P. ; Shahbandeh, M. ; Tomasella, L. ; Wang, X. ; Yan, S. ; Zhang, J. ; Zhang, T. ; Stritzinger, M. D. / SN 2020wnt : a slow-evolving carbon-rich superluminous supernova with no O II lines and a bumpy light curve. In: Monthly Notices of the Royal Astronomical Society. 2022 ; Vol. 517, No. 2. pp. 2056-2075.

Bibtex

@article{3ee1f69e4202430594920113a41fa12b,
title = "SN 2020wnt: a slow-evolving carbon-rich superluminous supernova with no O II lines and a bumpy light curve",
abstract = "We present the analysis of SN 2020wnt, an unusual hydrogen-poor superluminous supernova (SLSN-I), at a redshift of 0.032. The light curves of SN 2020wnt are characterized by an early bump lasting similar to 5 d, followed by a bright main peak. The SN reaches a peak absolute magnitude of M-r(max) = -20.52 +/- 0.03 mag at similar to 77.5 d from explosion. This magnitude is at the lower end of the luminosity distribution of SLSNe-I, but the rise-time is one of the longest reported to date. Unlike other SLSNe-I, the spectra of SN 2020wnt do not show O II, but strong lines of C II and Si II are detected. Spectroscopically, SN 2020wnt resembles the Type Ic SN 2007gr, but its evolution is significantly slower. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2020wnt luminosity can be explained by radioactive powering. The progenitor of SN 2020wnt is likely a massive and extended star with a pre-SN mass of 80 M-circle dot and a pre-SN radius of 15 R-circle dot that experiences a very energetic explosion of 45 x 10(51) erg, producing 4 M-circle dot of Ni-56. In this framework, the first peak results from a post-shock cooling phase for an extended progenitor, and the luminous main peak is due to a large nickel production. These characteristics are compatible with the pair-instability SN scenario. We note, however, that a significant contribution of interaction with circumstellar material cannot be ruled out.",
keywords = "supernovae: general, supernovae: individual: SN 2020wnt, MASS-METALLICITY RELATION, CORE COLLAPSE SUPERNOVAE, CIRCUMSTELLAR MEDIUM, LUMINOUS SUPERNOVA, INFRARED ECHOES, NEBULAR SPECTRA, IA SUPERNOVAE, IC SUPERNOVAE, HOST-GALAXY, EMISSION",
author = "Gutierrez, {C. P.} and A. Pastorello and M. Bersten and S. Benetti and M. Orellana and A. Fiore and E. Karamehmetoglu and T. Kravtsov and A. Reguitti and Reynolds, {T. M.} and G. Valerin and P. Mazzali and M. Sullivan and Y-Z Cai and N. Elias-Rosa and M. Fraser and Hsiao, {E. Y.} and E. Kankare and R. Kotak and H. Kuncarayakti and Z. Li and S. Mattila and J. Mo and S. Moran and P. Ochner and M. Shahbandeh and L. Tomasella and X. Wang and S. Yan and J. Zhang and T. Zhang and Stritzinger, {M. D.}",
year = "2022",
month = oct,
day = "17",
doi = "10.1093/mnras/stac2747",
language = "English",
volume = "517",
pages = "2056--2075",
journal = "Royal Astronomical Society. Monthly Notices",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "2",

}

RIS

TY - JOUR

T1 - SN 2020wnt

T2 - a slow-evolving carbon-rich superluminous supernova with no O II lines and a bumpy light curve

AU - Gutierrez, C. P.

AU - Pastorello, A.

AU - Bersten, M.

AU - Benetti, S.

AU - Orellana, M.

AU - Fiore, A.

AU - Karamehmetoglu, E.

AU - Kravtsov, T.

AU - Reguitti, A.

AU - Reynolds, T. M.

AU - Valerin, G.

AU - Mazzali, P.

AU - Sullivan, M.

AU - Cai, Y-Z

AU - Elias-Rosa, N.

AU - Fraser, M.

AU - Hsiao, E. Y.

AU - Kankare, E.

AU - Kotak, R.

AU - Kuncarayakti, H.

AU - Li, Z.

AU - Mattila, S.

AU - Mo, J.

AU - Moran, S.

AU - Ochner, P.

AU - Shahbandeh, M.

AU - Tomasella, L.

AU - Wang, X.

AU - Yan, S.

AU - Zhang, J.

AU - Zhang, T.

AU - Stritzinger, M. D.

PY - 2022/10/17

Y1 - 2022/10/17

N2 - We present the analysis of SN 2020wnt, an unusual hydrogen-poor superluminous supernova (SLSN-I), at a redshift of 0.032. The light curves of SN 2020wnt are characterized by an early bump lasting similar to 5 d, followed by a bright main peak. The SN reaches a peak absolute magnitude of M-r(max) = -20.52 +/- 0.03 mag at similar to 77.5 d from explosion. This magnitude is at the lower end of the luminosity distribution of SLSNe-I, but the rise-time is one of the longest reported to date. Unlike other SLSNe-I, the spectra of SN 2020wnt do not show O II, but strong lines of C II and Si II are detected. Spectroscopically, SN 2020wnt resembles the Type Ic SN 2007gr, but its evolution is significantly slower. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2020wnt luminosity can be explained by radioactive powering. The progenitor of SN 2020wnt is likely a massive and extended star with a pre-SN mass of 80 M-circle dot and a pre-SN radius of 15 R-circle dot that experiences a very energetic explosion of 45 x 10(51) erg, producing 4 M-circle dot of Ni-56. In this framework, the first peak results from a post-shock cooling phase for an extended progenitor, and the luminous main peak is due to a large nickel production. These characteristics are compatible with the pair-instability SN scenario. We note, however, that a significant contribution of interaction with circumstellar material cannot be ruled out.

AB - We present the analysis of SN 2020wnt, an unusual hydrogen-poor superluminous supernova (SLSN-I), at a redshift of 0.032. The light curves of SN 2020wnt are characterized by an early bump lasting similar to 5 d, followed by a bright main peak. The SN reaches a peak absolute magnitude of M-r(max) = -20.52 +/- 0.03 mag at similar to 77.5 d from explosion. This magnitude is at the lower end of the luminosity distribution of SLSNe-I, but the rise-time is one of the longest reported to date. Unlike other SLSNe-I, the spectra of SN 2020wnt do not show O II, but strong lines of C II and Si II are detected. Spectroscopically, SN 2020wnt resembles the Type Ic SN 2007gr, but its evolution is significantly slower. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2020wnt luminosity can be explained by radioactive powering. The progenitor of SN 2020wnt is likely a massive and extended star with a pre-SN mass of 80 M-circle dot and a pre-SN radius of 15 R-circle dot that experiences a very energetic explosion of 45 x 10(51) erg, producing 4 M-circle dot of Ni-56. In this framework, the first peak results from a post-shock cooling phase for an extended progenitor, and the luminous main peak is due to a large nickel production. These characteristics are compatible with the pair-instability SN scenario. We note, however, that a significant contribution of interaction with circumstellar material cannot be ruled out.

KW - supernovae: general

KW - supernovae: individual: SN 2020wnt

KW - MASS-METALLICITY RELATION

KW - CORE COLLAPSE SUPERNOVAE

KW - CIRCUMSTELLAR MEDIUM

KW - LUMINOUS SUPERNOVA

KW - INFRARED ECHOES

KW - NEBULAR SPECTRA

KW - IA SUPERNOVAE

KW - IC SUPERNOVAE

KW - HOST-GALAXY

KW - EMISSION

U2 - 10.1093/mnras/stac2747

DO - 10.1093/mnras/stac2747

M3 - Journal article

VL - 517

SP - 2056

EP - 2075

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

SN - 0035-8711

IS - 2

ER -

ID: 324369426