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Andrews, JE, Sand, DJ, Valenti, S, Smith, N, Dastidar, R, Sahu, DK, Misra, K, Singh, A, Hiramatsu, D, Brown, PJ, Hosseinzadeh, G, Wyatt, S, Vinko, J, Anupama, GC, Arcavi, I, Ashall, C, Benetti, S, Berton, M, Bostroem, KA, Bulla, M , Burke, J, Chen, S, Chomiuk, L, Cikota, A, Congiu, E, Cseh, B, Davis, S, Elias-Rosa, N, Faran, T, Fraser, M, Galbany, L, Gall, C, Gal-Yam, A, Gangopadhyay, A, Gromadzki, M, Haislip, J, Howell, DA, Hsiao, EY, Inserra, C, Kankare, E, Kuncarayakti, H, Kouprianov, V, Kumar, B, Li, X, Lin, H, Maguire, K, Mazzali, PA, McCully, C, Milne, P, Mo, J, Morrell, N, Nicholl, M, Ochner, P, Olivares, F, Pastorello, A, Patat, F, Phillips, M, Pignata, G, Prentice, S, Reguitti, A, Reichart, DE, Rodriguez, O, Rui, L, Sanwal, P, Sarneczky, K, Shahbandeh, M, Singh, M, Smartt, S, Strader, J, Stritzinger, MD, Szakats, R, Tartaglia, L, Wang, H, Wang, L, Wang, X, Wheeler, JC, Xiang, D, Yaron, O, Young, DR and Zhang, J (2019) SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries. Astrophysical Journal, 885 (1). ISSN 0004-637X
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SN 2017gmr An Energetic Type II-P Supernova with Asymmetries.pdf - Accepted Version Download (1MB) | Preview |
Abstract
We present high-cadence UV, optical, and near-infrared data on the luminous Type II-P supernova SN 2017gmr from hours after discovery through the first 180 days. SN 2017gmr does not show signs of narrow, high-ionization emission lines in the early optical spectra, yet the optical light-curve evolution suggests that an extra energy source from circumstellar medium (CSM) interaction must be present for at least 2 days after explosion. Modeling of the early light curve indicates a ~500 R ⊙ progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate that up to 0.130 ± 0.026 M ⊙ of 56Ni are present, if the light curve is solely powered by radioactive decay, although the 56Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multipeaked emission lines of Hα and [O i] emerge after day 154, as a result of either an asymmetric explosion or asymmetries in the CSM. The lack of narrow lines within the first 2 days of explosion in the likely presence of CSM interaction may be an example of close, dense, asymmetric CSM that is quickly enveloped by the spherical supernova ejecta.
| Item Type: | Article |
|---|---|
| Uncontrolled Keywords: | 0201 Astronomical and Space Sciences, 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics, 0306 Physical Chemistry (incl. Structural) |
| Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
| Divisions: | Astrophysics Research Institute |
| Publisher: | American Astronomical Society; IOP Publishing |
| Related URLs: | |
| Date Deposited: | 06 Jan 2020 10:31 |
| Last Modified: | 04 Sep 2021 08:14 |
| DOI or ID number: | 10.3847/1538-4357/ab43e3 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/11943 |
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