A1 Refereed original research article in a scientific journal

Statistical Properties of the Nebular Spectra of 103 Stripped-envelope Core-collapse Supernovae*




AuthorsFang Qiliang, Maeda Keiichi, Kuncarayakti Hanindyo, Tanaka Masaomi, Kawabata Koji S., Hattori Takashi, Aoki Kentaro, Moriya Takashi J., Yamanaka Masayuki

PublisherIOP Publishing Ltd

Publication year2022

JournalAstrophysical Journal

Journal name in sourceASTROPHYSICAL JOURNAL

Journal acronymASTROPHYS J

Article number 151

Volume928

Issue2

Number of pages31

ISSN0004-637X

eISSN1538-4357

DOIhttps://doi.org/10.3847/1538-4357/ac4f60

Web address https://iopscience.iop.org/article/10.3847/1538-4357/ac4f60

Self-archived copy’s web addresshttps://research.utu.fi/converis/portal/detail/Publication/175242262

Preprint addresshttps://arxiv.org/abs/2201.11467


Abstract
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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