Close, bright, and boxy: the superluminous SN 2018hti

A. Fiore; S. Benetti; M. Nicholl; A. Reguitti; E. Cappellaro; S. Campana; S. Bose; E. Paraskeva; E. Berger; T. M. Bravo; J. Burke; Y. -Z. Cai; T. -W. Chen; P. Chen; R. Ciolfi; S. Dong; S. Gomez; M. Gromadzki; C. P. Gutiérrez; D. Hiramatsu; G. Hosseinzadeh; D. A. Howell; A. Jerkstrand; E. Kankare; A. Kozyreva; K. Maguire; C. McCully; P. Ochner; C. Pellegrino; G. Pignata; R. S. Post; N. Elias-Rosa; M. Shahbandeh; S. Schuldt; B. P. Thomas; L. Tomasella; J. Vinkó; C. Vogl; J. C. Wheeler; D. R. Young

doi:10.1093/mnras/stac744

Close, bright, and boxy: the superluminous SN 2018hti

A. Fiore, S. Benetti, M. Nicholl, A. Reguitti, E. Cappellaro, S. Campana, S. Bose, E. Paraskeva, E. Berger, T. M. Bravo, J. Burke, Y. -Z. Cai, T. -W. Chen, P. Chen, R. Ciolfi, S. Dong, S. Gomez, M. Gromadzki, C. P. Gutiérrez, D. HiramatsuG. Hosseinzadeh, D. A. Howell, A. Jerkstrand, E. Kankare, A. Kozyreva, K. Maguire, C. McCully, P. Ochner, C. Pellegrino, G. Pignata, R. S. Post, N. Elias-Rosa, M. Shahbandeh, S. Schuldt, B. P. Thomas, L. Tomasella, J. Vinkó, C. Vogl, J. C. Wheeler, D. R. Young

Physics and Astronomy

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Abstract

SN 2018hti was a very nearby (z = 0.0614) superluminous supernova with an exceedingly bright absolute magnitude of -21.7 mag in r band at maximum. The densely sampled pre-maximum light curves of SN 2018hti show a slow luminosity evolution and constrain the rise time to ~50 rest-frame d. We fitted synthetic light curves to the photometry to infer the physical parameters of the explosion of SN 2018hti for both the magnetar and the CSM-interaction scenarios. We conclude that one of two mechanisms could be powering the luminosity of SN 2018hti; interaction with ~10 M_☉ of circumstellar material or a magnetar with a magnetic field of B_p~ 1.3 × 10¹³ G, and initial period of P_spin~ 1.8 ms. From the nebular spectrum modelling we infer that SN 2018hti likely results from the explosion of a 40_☉ progenitor star.

Original language	English
Pages (from-to)	4484–4502
Number of pages	19
Journal	Monthly Notices of the Royal Astronomical Society
Volume	512
Issue number	3
Early online date	17 Mar 2022
DOIs	https://doi.org/10.1093/mnras/stac744
Publication status	Published - May 2022

Keywords

supernovae: general
supernovae: individual: SN 2018hti

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10.1093/mnras/stac744

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This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2022 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
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Fiore, A., Benetti, S., Nicholl, M., Reguitti, A., Cappellaro, E., Campana, S., Bose, S., Paraskeva, E., Berger, E., Bravo, T. M., Burke, J., Cai, Y. .-Z., Chen, T. .-W., Chen, P., Ciolfi, R., Dong, S., Gomez, S., Gromadzki, M., Gutiérrez, C. P., ... Young, D. R. (2022). Close, bright, and boxy: the superluminous SN 2018hti. Monthly Notices of the Royal Astronomical Society, 512(3), 4484–4502. https://doi.org/10.1093/mnras/stac744

@article{3799993c87c24ca0b4a2bd59fe47ec79,

title = "Close, bright, and boxy: the superluminous SN 2018hti",

abstract = "SN 2018hti was a very nearby (z = 0.0614) superluminous supernova with an exceedingly bright absolute magnitude of -21.7 mag in r band at maximum. The densely sampled pre-maximum light curves of SN 2018hti show a slow luminosity evolution and constrain the rise time to ~50 rest-frame d. We fitted synthetic light curves to the photometry to infer the physical parameters of the explosion of SN 2018hti for both the magnetar and the CSM-interaction scenarios. We conclude that one of two mechanisms could be powering the luminosity of SN 2018hti; interaction with ~10 M☉ of circumstellar material or a magnetar with a magnetic field of Bp~ 1.3 × 1013 G, and initial period of Pspin~ 1.8 ms. From the nebular spectrum modelling we infer that SN 2018hti likely results from the explosion of a 40☉ progenitor star.",

keywords = "supernovae: general, supernovae: individual: SN 2018hti",

author = "A. Fiore and S. Benetti and M. Nicholl and A. Reguitti and E. Cappellaro and S. Campana and S. Bose and E. Paraskeva and E. Berger and Bravo, {T. M.} and J. Burke and Cai, {Y. -Z.} and Chen, {T. -W.} and P. Chen and R. Ciolfi and S. Dong and S. Gomez and M. Gromadzki and Guti{\'e}rrez, {C. P.} and D. Hiramatsu and G. Hosseinzadeh and Howell, {D. A.} and A. Jerkstrand and E. Kankare and A. Kozyreva and K. Maguire and C. McCully and P. Ochner and C. Pellegrino and G. Pignata and Post, {R. S.} and N. Elias-Rosa and M. Shahbandeh and S. Schuldt and Thomas, {B. P.} and L. Tomasella and J. Vink{\'o} and C. Vogl and Wheeler, {J. C.} and Young, {D. R.}",

year = "2022",

month = may,

doi = "10.1093/mnras/stac744",

language = "English",

volume = "512",

pages = "4484–4502",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "SIPRI/Oxford University Press",

number = "3",

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Fiore, A, Benetti, S, Nicholl, M, Reguitti, A, Cappellaro, E, Campana, S, Bose, S, Paraskeva, E, Berger, E, Bravo, TM, Burke, J, Cai, Y-Z, Chen, T-W, Chen, P, Ciolfi, R, Dong, S, Gomez, S, Gromadzki, M, Gutiérrez, CP, Hiramatsu, D, Hosseinzadeh, G, Howell, DA, Jerkstrand, A, Kankare, E, Kozyreva, A, Maguire, K, McCully, C, Ochner, P, Pellegrino, C, Pignata, G, Post, RS, Elias-Rosa, N, Shahbandeh, M, Schuldt, S, Thomas, BP, Tomasella, L, Vinkó, J, Vogl, C, Wheeler, JC & Young, DR 2022, 'Close, bright, and boxy: the superluminous SN 2018hti', Monthly Notices of the Royal Astronomical Society, vol. 512, no. 3, pp. 4484–4502. https://doi.org/10.1093/mnras/stac744

TY - JOUR

T1 - Close, bright, and boxy

T2 - the superluminous SN 2018hti

AU - Fiore, A.

AU - Benetti, S.

AU - Nicholl, M.

AU - Reguitti, A.

AU - Cappellaro, E.

AU - Campana, S.

AU - Bose, S.

AU - Paraskeva, E.

AU - Berger, E.

AU - Bravo, T. M.

AU - Burke, J.

AU - Cai, Y. -Z.

AU - Chen, T. -W.

AU - Chen, P.

AU - Ciolfi, R.

AU - Dong, S.

AU - Gomez, S.

AU - Gromadzki, M.

AU - Gutiérrez, C. P.

AU - Hiramatsu, D.

AU - Hosseinzadeh, G.

AU - Howell, D. A.

AU - Jerkstrand, A.

AU - Kankare, E.

AU - Kozyreva, A.

AU - Maguire, K.

AU - McCully, C.

AU - Ochner, P.

AU - Pellegrino, C.

AU - Pignata, G.

AU - Post, R. S.

AU - Elias-Rosa, N.

AU - Shahbandeh, M.

AU - Schuldt, S.

AU - Thomas, B. P.

AU - Tomasella, L.

AU - Vinkó, J.

AU - Vogl, C.

AU - Wheeler, J. C.

AU - Young, D. R.

PY - 2022/5

Y1 - 2022/5

N2 - SN 2018hti was a very nearby (z = 0.0614) superluminous supernova with an exceedingly bright absolute magnitude of -21.7 mag in r band at maximum. The densely sampled pre-maximum light curves of SN 2018hti show a slow luminosity evolution and constrain the rise time to ~50 rest-frame d. We fitted synthetic light curves to the photometry to infer the physical parameters of the explosion of SN 2018hti for both the magnetar and the CSM-interaction scenarios. We conclude that one of two mechanisms could be powering the luminosity of SN 2018hti; interaction with ~10 M☉ of circumstellar material or a magnetar with a magnetic field of Bp~ 1.3 × 1013 G, and initial period of Pspin~ 1.8 ms. From the nebular spectrum modelling we infer that SN 2018hti likely results from the explosion of a 40☉ progenitor star.

AB - SN 2018hti was a very nearby (z = 0.0614) superluminous supernova with an exceedingly bright absolute magnitude of -21.7 mag in r band at maximum. The densely sampled pre-maximum light curves of SN 2018hti show a slow luminosity evolution and constrain the rise time to ~50 rest-frame d. We fitted synthetic light curves to the photometry to infer the physical parameters of the explosion of SN 2018hti for both the magnetar and the CSM-interaction scenarios. We conclude that one of two mechanisms could be powering the luminosity of SN 2018hti; interaction with ~10 M☉ of circumstellar material or a magnetar with a magnetic field of Bp~ 1.3 × 1013 G, and initial period of Pspin~ 1.8 ms. From the nebular spectrum modelling we infer that SN 2018hti likely results from the explosion of a 40☉ progenitor star.

KW - supernovae: general

KW - supernovae: individual: SN 2018hti

U2 - 10.1093/mnras/stac744

DO - 10.1093/mnras/stac744

M3 - Article

SN - 0035-8711

VL - 512

SP - 4484

EP - 4502

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Close, bright, and boxy: the superluminous SN 2018hti

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Keywords

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