Refereed journal article or data article (A1)
Statistical Properties of the Nebular Spectra of 103 Stripped-envelope Core-collapse Supernovae*
List of Authors: Fang Qiliang, Maeda Keiichi, Kuncarayakti Hanindyo, Tanaka Masaomi, Kawabata Koji S., Hattori Takashi, Aoki Kentaro, Moriya Takashi J., Yamanaka Masayuki
Publisher: IOP Publishing Ltd
Publication year: 2022
Journal: Astrophysical Journal
Journal name in source: ASTROPHYSICAL JOURNAL
Journal acronym: ASTROPHYS J
Volume number: 928
Issue number: 2
Number of pages: 31
ISSN: 0004-637X
eISSN: 1538-4357
DOI: http://dx.doi.org/10.3847/1538-4357/ac4f60
URL: https://iopscience.iop.org/article/10.3847/1538-4357/ac4f60
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/175242262
We present an analysis of the nebular spectra of 103 stripped-envelope (SE) supernovae (SNe) collected from the literature and observed with the Subaru Telescope from 2002 to 2012, focusing on [O i] lambda lambda 6300, 6363. The line profile and width of [O i] are employed to infer the ejecta geometry and the expansion velocity of the inner core; these two measurements are then compared with the SN subtypes, and further with the [O i]/[Ca ii] ratio, which is used as an indicator of the progenitor CO core mass. Based on the best-fit results of the [O i] profile, the objects are classified into different morphological groups, and we conclude that the deviation from spherical symmetry is a common feature for all types of SESNe. There is a hint (at the similar to 1 sigma level) that the distributions of the line profile fractions are different between canonical SESNe and broad-line SNe Ic. A correlation between [O i] width and [O i]/[Ca ii] is discerned, indicating that the oxygen-rich material tends to expand faster for objects with a more massive CO core. Such a correlation can be utilized to constrain the relation between the progenitor mass and the kinetic energy of the explosion. Further, when [O i]/[Ca ii] increases, the fraction of objects with Gaussian [O i] profile increases, while those with double-peaked profile decreases. This phenomenon connects ejecta geometry and the progenitor CO core mass.
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