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Title: Investigating the properties of stripped-envelope supernovae; what are the implications for their progenitors?
Authors: Prentice, SJ
Ashall, C
James, PA
Short, L
Mazzali, PA
Bersier, D
Crowther, PA
Barbarino, C
Chen, TW
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
Olivares, F
Piascik, AS
Pignata, G
Reichart, DE
Rest, A
Reynolds, T
Saario, JLO
Schulze, S
Smartt, SJ
Smith, KW
Sollerman, J
Stalder, B
Sullivan, M
Taddia, F
Valenti, S
Vergani, SD
Williams, SC
Young, DR
First Published: 7-Dec-2018
Publisher: Oxford University Press (OUP), Royal Astronomical Society
Citation: Monthly Notices of the Royal Astronomical Society, 2019, 485 (2), pp. 1559-1578
Abstract: We present observations and analysis of 18 stripped-envelope supernovae observed during 2013–2018. This sample consists of five H/He-rich SNe, six H-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 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 M⊙. The bolometric light curve properties are examined in combination with those of other SE events from the literature. The resulting data set 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 ∼1.2–11 M⊙, considerably greater than any other subtype. For all SE–SNe <Mej> = 2.8 ± 1.5 M⊙ which further strengthens the evidence that SE–SNe arise from low-mass progenitors which are typically <5 M⊙ at the time of explosion, again suggesting MZAMS <25 M⊙. The low <Mej> and lack of clear bimodality in the distribution implies <30 M⊙ progenitors and that envelope stripping via binary interaction is the dominant evolutionary pathway of these SNe.
DOI Link: 10.1093/mnras/sty3399
ISSN: 0035-8711
eISSN: 1365-2966
Version: Publisher Version
Status: Peer-reviewed
Type: Journal Article
Rights: Copyright © 2018, Oxford University Press (OUP), Royal Astronomical Society. Deposited with reference to the publisher’s open access archiving policy. (
Description: Supplementary data are available at MNRAS online. Figre S1: (Top left) The spectra of SN 2016P without host emission line removal. (Top right) Comparison with Ic-4 SNe 2002ap. The lines of SN 2002ap are much broader and at higher velocity. (Lower left) Comparison with SN 1994I, the major features align, although the velocities of SN 1994I are typically higher (except for Na i D). (Lower right) Comparison with Ic-7 SN 2007 gr. The velocities are broadly consistent but there are more features in the spectra SN 2007gr, albeit with a higher S/N Figure S2: The spectra of SN 2013F, epochs are relative to maximum light. Figure S3: Spectroscopic observations of SN 2013bb. Figure S4: Spectroscopic observations of SN 2013ek. Figure S5: Spectroscopic observations of SN 2015ah. Figure S6: Spectroscopic observations of SN 2015ap. Figure S7: Spectroscopic observations of SN 2016P. Figure S8: Spectroscopic observations of SN 2016frp. Figure S9: Spectroscopic observations of SN 2016iae. Figure S10: Spectroscopic observations of SN 2016jdw. Figure S11: Spectroscopic observations of SN 2017bgu. Figure S12: Spectroscopic observations of SN 2017dcc. Figure S13: Spectroscopic observations of SN 2017gpn. Figure S14: Spectroscopic observations of SN 2017ifh. Figure S15: Spectroscopic observations of SN 2017ixz. Figure S16: Spectroscopic observations of SN 2018ie. Figure S17: Spectroscopic observations of SN 2018cbz. Table S1: 4000–10000 Å bolometric light curve properties of SNe in the extended P16 sample. Table S2: Derived E(B − V)host for SNe in P16 and updated parameters Table S3: Table of δm100 values for the extended P16 sample. Table S4: Mej of the extended P16 sample SNe and comparison with Mej from spectral modelling and hydrodynamics codes.
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