The classification of supernovae (SNe) has remained a challenging task in astrophysics since the first type distinction was made in 1941 by (Minkowski 1941). Minkowski split SNe into two groups: Type I spectra do not have any Hydrogen features, while Type II spectra exhibit strong Hydrogen features. Since then, SNe classification has developed more complexity as the number of observed spectra has increased, along higher quality of observing instruments. Figure 1 illustrates the basic classification scheme, excluding unique spectra that might define their own subtypes.

In this paper, we focus on Type I SNe, specifically types Ib, Ic, broad line Ic (Ic-BL), and IIb. These non Type Ia SNe are generally less studied than Type Ia because they are not used as standard candles. Type Ib SNe are generally characterized by the presence of a strong HeI line, while Type Ic spectra lack this feature. Type IIb spectra resemble Ib spectra, but with the presence of a weak Hydrogen line at early phases. More information on the historical classification of SNe can be found in (Filippenko 1997) or (Matheson 2001), and more recent discussion can be found in (Modjaz 2014), (Liu 2016), and (Modjaz 2016). These four SNe types are examples of stripped-envelope core-collapse super novae (SESNe). A SESNe is classified by the lack of Hydrogen layers, and often Helium layers, in the progenitor star. The progenitors lose their outer shells either through strong winds woo