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iPTF16abc and the population of Type Ia supernovae: comparing the photospheric, transitional, and nebular phases
Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).ORCID iD: 0000-0002-4163-4996
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).ORCID iD: 0000-0001-9454-4639
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Number of Authors: 92018 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 480, no 2, p. 1445-1456Article in journal (Refereed) Published
Abstract [en]

Key information about the progenitor system and the explosion mechanism of Type la supernovae (SNe Ia) can be obtained from early observations, within a few days from explosion. iPTF16abc was discovered as a young SN la with excellent early time data. Here, we present photometry and spectroscopy of the SN in the nebular phase. A comparison of the early time data with a sample of SNe la shows distinct features, differing from normal SNe la at early phases but similar to normal SNe Ia at a few weeks after maximum light (i.e. the transitional phase) and well into the nebular phase. The transparency time-scales (t(0)) for this sample of SNe Ia range between similar to 25 and 41 d indicating a diversity in the ejecta masses. t(0) also weakly correlates with the peak bolometric luminosity, consistent with the interpretation that SNe with higher ejecta masses would produce more Ni-56. Comparing the to and the maximum luminosity, L-max distribution of a sample of SNe Ia to predictions from a wide range of explosion models we find an indication that the sub-Chandrasekhar mass models span the range of observed values. However, the bright end of the distribution can be better explained by Chandrasekhar mass delayed detonation models, hinting at multiple progenitor channels to explain the observed bolometric properties of SNe Ia. iPTF16abc appears to be consistent with the predictions from the M-ch models.

Place, publisher, year, edition, pages
2018. Vol. 480, no 2, p. 1445-1456
Keywords [en]
supernovae: general, supernova: individual (iPTF16abc)
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-162923DOI: 10.1093/mnras/sty1908ISI: 000449614800002OAI: oai:DiVA.org:su-162923DiVA, id: diva2:1272128
Available from: 2018-12-18 Created: 2018-12-18 Last updated: 2018-12-18Bibliographically approved

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Dhawan, SuhailBulla, MattiaGoobar, ArielLunnan, RagnhildFransson, ClaesPapadogiannakis, Seméli
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Department of PhysicsThe Oskar Klein Centre for Cosmo Particle Physics (OKC)Department of Astronomy
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