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Prentice, SJ, Ashall, C, Mazzali, PA, Zhang, J-J, James, PA, Wang, X-F, Vinko, J, Percival, SM, Short, L, Piascik, A, Huang, F, Mo, J, Rui, L-M, Wang, J-G, Xiang, D-F, Xin, Y-X, Yi, W-M, Yu, X-G, Zhai, Q, Zhang, T-M , Hosseinzadeh, G, Howell, DA, McCully, C, Valenti, S, Cseh, B, Hanyecz, O, Kriskovics, L, Pal, A, Sarneczky, K, Sodor, A, Szakats, R, Szekely, P, Varga-Verebelyi, E, Vida, K, Bradac, M, Reichart, DE, Sand, D and Tartaglia, L (2018) SN 2016coi/ASASSN-16fp: an example of residual helium in a type Ic supernova? Monthly Notices of the Royal Astronomical Society, 478 (3). pp. 4162-4192. ISSN 0035-8711
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SN 2016coi ASASSN-16fp an example of residual helium in a type Ic supernova.pdf - Published Version Download (10MB) | Preview |
Abstract
The optical observations of Ic-4 supernova (SN) 2016coi/ASASSN-16fp, from ∼2 to ∼450 d after explosion, are presented along with analysis of its physical properties. The SN shows the broad lines associated with SNe Ic-3/4 but with a key difference. The early spectra display a strong absorption feature at ∼5400 Å which is not seen in other SNe Ic-3/4 at this epoch. This feature has been attributed to He I in the literature. Spectral modelling of the SN in the early photospheric phase suggests the presence of residual He in a C/O dominated shell. However, the behaviour of the He I lines is unusual when compared with He-rich SNe, showing relatively low velocities and weakening rather than strengthening over time. The SN is found to rise to peak ∼16 d after core-collapse reaching a bolometric luminosity of Lp∼3 × 1042 erg s−1. Spectral models, including the nebular epoch, show that the SN ejected 2.5–4 M⊙ of material, with ∼1.5 M⊙ below 5000 km s−1, and with a kinetic energy of (4.5–7) × 1051 erg. The explosion synthesized ∼0.14 M⊙ of 56Ni. There are significant uncertainties in E(B − V)host and the distance, however, which will affect Lp and MNi. SN 2016coi exploded in a host similar to the Large Magellanic Cloud (LMC) and away from star-forming regions. The properties of the SN and the host-galaxy suggest that the progenitor had MZAMS of 23–28 M⊙ and was stripped almost entirely down to its C/O core at explosion.
| Item Type: | Article |
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| Additional Information: | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2018 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
| Uncontrolled Keywords: | 0201 Astronomical And Space Sciences |
| Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
| Divisions: | Astrophysics Research Institute |
| Publisher: | Oxford University Press |
| Related URLs: | |
| Date Deposited: | 17 Oct 2018 08:45 |
| Last Modified: | 04 Sep 2021 02:20 |
| DOI or ID number: | 10.1093/mnras/sty1223 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/9493 |
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