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Investigating the properties of stripped-envelope supernovae, what are the implications for their progenitors?

Prentice, SJ, Ashall, C, James, PA, Short, L, Mazzali, PA, Bersier, D, Crowther, PA, Barbarino, C, Chen, T-W, Copperwheat, CM, Darnley, MJ, Denneau, L, Elias-Rosa, N, Fraser, M, Galbany, L, Gal-Yam, A, Harmanen, J, Howell, DA, Hosseinzadeh, G, Inserra, C , Kankare, E, Karamehmetoglu, E, Lamb, GP, Limongi, M, Maguire, K, McCully, C, Oliveres E, F, Piascik, AS, Pignata, G, Reichart, DE, Reynolds, ART, Rodríguez, Ó, Saario, JLO, Schulze, S, Smartt, SJ, Smith, KW, Sollerman, J, Stalder, B, Sullivan, M, Taddia, F, Valenti, S, Vergani, SD, Williams, SC and Young, DR Investigating the properties of stripped-envelope supernovae, what are the implications for their progenitors? Monthly Notices of the Royal Astronomical Society. ISSN 0035-8711 (Accepted)

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Abstract

We present observations and analysis of 18 stripped-envelope supernovae observed during 2013 -- 2018. This sample consists of 5 H/He-rich SNe, 6 H-poor/He-rich SNe, 3 narrow lined SNe Ic and 4 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 56Ni and ejecta masses (MNi and Mej). 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 $<20$ Msun. The bolometric light curve properties are examined in combination with those of other SE events from the literature. The resulting dataset gives the Mej distribution for 80 SE-SNe, the largest such sample in the literature to date, and shows that SNe Ib have the lowest median Mej, 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 Mej, ranging from $\sim 1.2 - 11$ Msun, considerably greater than any other subtype. For all SE-SNe $<$Mej$>=2.8\pm{1.5}$ Msun which further strengthens the evidence that SE-SNe arise from low mass progenitors which are typically $<5$ Msun at the time of explosion, again suggesting Mzams $<25$ Msun. The low $<$Mej$>$ and lack of clear bimodality in the distribution implies $<30$ Msun progenitors and that envelope stripping via binary interaction is the dominant evolutionary pathway of these SNe.

Item Type: Article
Uncontrolled Keywords: astro-ph.HE; astro-ph.HE
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: Oxford University Press
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Date Deposited: 18 Dec 2018 09:55
Last Modified: 18 Dec 2018 09:58
URI: http://researchonline.ljmu.ac.uk/id/eprint/9833

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