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Supernovae (SNe) with photospheric spectra devoid of Hydrogen and Heliumfeatures are generally classified as Type Ic SNe (SNe Ic). However, there isongoing debate as to whether Helium can be hidden in the ejecta of SNe Ic (thatis, Helium is present in the ejecta, but produces no obvious features in thespectra). We present the first application of the fast, 1-D radiative transfercode TARDIS to a SN Ic, and we investigate the question of how much Helium canbe hidden in the outer layers of the SN Ic ejecta. We generate TARDIS modelsfor the nearby, well-observed, and extensively modeled SN Ic 1994I, and weperform a code comparison to a different, well-established Monte Carlo basedradiation transfer code. The code comparison shows that TARDIS producesconsistent synthetic spectra for identical ejecta models of SN1994I. Inaddition, we perform a systematic experiment of adding outer He shells ofvarying masses to our SN1994I models. We find that an outer He shell of only$0.05M_{\odot}$ produces strong optical and NIR He spectral features forSN1994I which are not present in observations, thus indicating that the SN1994Iejecta is almost fully He deficient compared to the He masses of typicalHe-rich SN progenitors. Finally we show that the He I $\lambda$20851 linepseudo equivalent width of our modeled spectra for SN1994I could be used toinfer the outer He shell mass which suggests that NIR spectral follow-up of SNeIc will be critical for addressing the hidden helium question for a statisticalsample of SNe Ic.

Modelling Type Ic Supernovae with TARDIS: Hidden Helium in SN1994I?