  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.
