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

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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 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 ${\sim}40\, \mathrm{M}_\odot$ 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

Space and Planetary Science
Astronomy and Astrophysics

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Close, bright, and boxy: the superluminous SN 2018hti
© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. This work is made available online in accordance with the publisher’s policies. Please refer to any applicable terms of use of the publisher.
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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{699b6da3aafb4ab19d194f2546acb990,

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 ${\sim}40\, \mathrm{M}_\odot$ progenitor star.",

keywords = "Space and Planetary Science, Astronomy and Astrophysics",

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 Y-Z Cai and T-W Chen 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 = "Oxford University Press",

number = "3",

}

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: 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 ${\sim}40\, \mathrm{M}_\odot$ 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 ${\sim}40\, \mathrm{M}_\odot$ progenitor star.

KW - Space and Planetary Science

KW - Astronomy and Astrophysics

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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