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SN 2017ivv: two years of evolution of a transitional Type II supernova

Gutiérrez, CP, Pastorello, A, Jerkstrand, A, Galbany, L, Sullivan, M, Anderson, JP, Taubenberger, S, Kuncarayakti, H, González-Gaitán, S, Wiseman, P, Inserra, C, Fraser, M, Maguire, K, Smartt, S, Müller-Bravo, TE, Arcavi, I, Benetti, S, Bersier, D, Bose, S, Bostroem, KA , Burke, J, Chen, P, Chen, T-W, Valle, MD, Dong, S, Gal-Yam, A, Gromadzki, M, Hiramatsu, D, Holoien, TW-S, Hosseinzadeh, G, Howell, DA, Kankare, E, Kochanek, CS, McCully, C, Nicholl, M, Pignata, G, Prieto, JL, Shappee, B, Taggart, K, Tomasella, L, Valenti, S and Young, DR (2020) SN 2017ivv: two years of evolution of a transitional Type II supernova. Monthly Notices of the Royal Astronomical Society, 499 (1). pp. 974-992. ISSN 0035-8711

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We present the photometric and spectroscopic evolution of the Type II supernova (SN II) SN 2017ivv (also known as ASASSN-17qp). Located in an extremely faint galaxy (M$_r=-10.3$ mag), SN 2017ivv shows an unprecedented evolution during the two years of observations. At early times, the light curve shows a fast rise ($\sim6-8$ days) to a peak of ${\rm M}^{\rm max}_{g}= -17.84$ mag, followed by a very rapid decline of $7.94\pm0.48$ mag per 100 days in the $V-$band. The extensive photometric coverage at late phases shows that the radioactive tail has two slopes, one steeper than that expected from the decay of $^{56}$Co (between 100 and 350 days), and another slower (after 450 days), probably produced by an additional energy source. From the bolometric light curve, we estimated that the amount of ejected $^{56}$Ni is $\sim0.059\pm0.003$ M$\odot$. The nebular spectra of SN 2017ivv show a remarkable transformation that allows the evolution to be split into three phases: (1) H$\alpha$ strong phase ($<200$ days); (2) H$\alpha$ weak phase (between 200 and 350 days); and (3) H$\alpha$ broad phase ($>500$ days). We find that the nebular analysis favours a binary progenitor and an asymmetric explosion. Finally, comparing the nebular spectra of SN 2017ivv to models suggests a progenitor with a zero-age main-sequence mass of 15 -- 17 \Msun.

Item Type: Article
Additional Information: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2020 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: 01 Apr 2021 12:40
Last Modified: 04 Sep 2021 05:39
DOI or ID number: 10.1093/mnras/staa2763
URI: https://researchonline.ljmu.ac.uk/id/eprint/14736
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