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Investigating the properties of stripped-envelope supernovae; what are the implications for their progenitors?
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Number of Authors: 452019 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 485, no 2, p. 1559-1578Article in journal (Refereed) Published
Abstract [en]

We present observations and analysis of 18 stripped-envelope supernovae observed during 2013-2018. This sample consists of five H/He-rich SNe, sixH-poor/He-rich SNe, three narrow lined SNe Ic, and four broad lined SNe Ic. The peak luminosity and characteristic time-scales of the bolometric light curves are calculated, and the light curves modelled to derive Ni-56 and ejecta masses (M-Ni and M-cj). Additionally, the temperature evolution and spectral line velocity curves of each SN are examined. Analysis of the [O I] line in the nebular phase of eight SNe suggests their progenitors had initial masses < 20 M-circle dot. The bolometric light curve properties are examined in combination with those of other SE events from the literature. The resulting data set gives the M-ej distribution for 80 SE-SNe, the largest such sample in the literature to date, and shows that SNe Ib have the lowest median M-ej, followed by narrow-lined SNe Ic, H/He-rich SNe, broad-lined SNe Ic, and finally gamma-ray burst SNe. SNe Ic-6/7 show the largest spread of M-ej ranging from similar to 1.2-11 M-circle dot, considerably greater than any other subtype. For all SE-SNe <M-ej> = 2.8 +/- 1.5 M-circle dot which further strengthens the evidence that SE-SNe arise from low-mass progenitors which are typically <5 M-circle dot at the time of explosion, again suggesting M-ZAMS < 25 M-circle dot. The low <M-ej> and lack of clear bimodality in the distribution implies < 30 M-circle dot progenitors and that envelope stripping via binary interaction is the dominant evolutionary pathway of these SNe.

Place, publisher, year, edition, pages
2019. Vol. 485, no 2, p. 1559-1578
Keywords [en]
Supernovae: general
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Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-172063DOI: 10.1093/mnras/sty3399ISI: 000474886200005OAI: oai:DiVA.org:su-172063DiVA, id: diva2:1345014
Available from: 2019-08-22 Created: 2019-08-22 Last updated: 2019-08-22Bibliographically approved

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Prentice, S. J.Barbarino, CristinaFraser, M.Inserra, C.Karamehmetoglu, EmirSchulze, S.Sollerman, JesperTaddia, Francesco
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Department of AstronomyThe Oskar Klein Centre for Cosmo Particle Physics (OKC)
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