The low-luminosity Type II SN 2016aqf: a well-monitored spectral evolution of the Ni/Fe abundance ratio

Müller-Bravo, Tomás E, Gutiérrez, Claudia P, Sullivan, Mark, Jerkstrand, Anders, Anderson, Joseph P, González-Gaitán, Santiago, Sollerman, Jesper, Arcavi, Iair, Burke, Jamison, Galbany, Lluís, Gal-Yam, Avishay, Gromadzki, Mariusz, Hiramatsu, Daichi, Hosseinzadeh, Griffin, Howell, D Andrew, Inserra, Cosimo ORCID: https://orcid.org/0000-0002-3968-4409, Kankare, Erki, Kozyreva, Alexandra, McCully, Curtis, Nicholl, Matt, Smartt, Stephen, Valenti, Stefano and Young, Dave R 2020. The low-luminosity Type II SN 2016aqf: a well-monitored spectral evolution of the Ni/Fe abundance ratio. Monthly Notices of the Royal Astronomical Society 497 (1) , pp. 361-377. 10.1093/mnras/staa1932

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Abstract

ABSTRACT Low-luminosity Type II supernovae (LL SNe II) make up the low explosion energy end of core-collapse SNe, but their study and physical understanding remain limited. We present SN2016aqf, an LL SN II with extensive spectral and photometric coverage. We measure a V-band peak magnitude of −14.58mag, a plateau duration of ∼100d, and an inferred 56Ni mass of 0.008 ± 0.002M. The peak bolometric luminosity, Lbol ≈ 1041.4 ergs−1, and its spectral evolution are typical of other SNe in the class. Using our late-time spectra, we measure the [OI] λλ6300, 6364 lines, which we compare against SN II spectral synthesismodelstoconstraintheprogenitorzero-agemain-sequencemass.Wefindthistobe12±3M.Ourextensivelate-time spectral coverage of the [FeII] λ7155 and [NiII] λ7378 lines permits a measurement of the Ni/Fe abundance ratio, a parameter sensitivetotheinnerprogenitorstructureandexplosionmechanismdynamics.Wemeasureaconstantabundanceratioevolution of 0.081+0.009 −0.010 and argue that the best epochs to measure the ratio are at∼200–300d after explosion. We place this measurement in the context of a large sample of SNe II and compare against various physical, light-curve, and spectral parameters, in search of trends that might allow indirect ways of constraining this ratio. We do not find correlations predicted by theoretical models; however, this may be the result of the exact choice of parameters and explosion mechanism in the models, the simplicity of them, and/or primordial contamination in the measured abundance ratio. Key words: techniques: photometric–spectroscopic telescopes–supernovae: individual: SN2016aqf–transients: supernovae.

Item Type:	Article
Date Type:	Published Online
Status:	Published
Schools:	Physics and Astronomy
Publisher:	Oxford University Press
ISSN:	0035-8711
Date of First Compliant Deposit:	18 September 2020
Date of Acceptance:	29 June 2020
Last Modified:	02 May 2023 13:50
URI:	https://orca.cardiff.ac.uk/id/eprint/134922

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