Observations and Spectral Modelling of the Narrow-Lined Type Ic SN 2017ein

TL;DR

This study models the spectral evolution of the narrow-lined Type Ic SN 2017ein, revealing a low-mass progenitor contrary to pre-supernova estimates, and provides insights into its explosion mechanics and ejecta asymmetry.

Contribution

It presents the first detailed spectral modeling of SN 2017ein across multiple phases, challenging previous high-mass progenitor assumptions with new nebular and photospheric data.

Findings

Ejected mass estimated at 1.2-2.0 M$_{\odot}$

$^{56}$Ni mass of 0.08-0.1 M$_{\odot}$

Inner ejecta asymmetry suggested by [OI] emission

Abstract

SN 2017ein is a narrow-lined Type Ic SN that was found to share a location with a point-like source in the face on spiral galaxy NGC 3938 in pre-supernova images, making SN 2017ein the first credible detection of a Type Ic progenitor. Results in the literature suggest this point-like source is likely a massive progenitor of 60-80 M$_{\odot}$, depending on if the source is a binary, a single star, or a compact cluster. Using new photometric and spectral data collected for 200 days, including several nebular spectra, we generate a consistent model covering the photospheric and nebular phase using a Monte Carlo radiation transport code. Photospheric phase modelling finds an ejected mass 1.2-2.0 M$_{\odot}$ with an $E_\mathrm{k}$ of $\sim(0.9 \pm0.2)\times 10^{51}$ erg, with approximately 1 M$_{\odot}$ of material below 5000 km s$^{-1}$ found from the nebular spectra. Both photospheric and nebular phase modelling suggests a $^{56}$Ni mass of 0.08-0.1 M$_{\odot}$. Modelling the [\OI] emission feature in the nebular spectra suggests the innermost ejecta is asymmetric. The modelling results favour a low mass progenitor of to 16-20 M$_{\odot}$, which is in disagreement with the pre-supernova derived high mass progenitor. This contradiction is likely due to the pre-supernova source not representing the actual progenitor.