  The classification of stripped-envelope supernovae (SE-SNe) is revisited
using modern data-sets. Spectra are analysed using an empirical method to
"blindly" categorise SNe according to spectral feature strength and appearance.
This method makes a clear distinction between SNe that are He-rich (IIb/Ib) and
He-poor (Ic) and further analysis is performed on each subgroup. For He-rich
SNe the presence of H becomes the focus. The strength, velocity, and ratio
between absorption and emission of H$\alpha$ is measured, along with additional
analysis of He I lines, in order to categorise the SNe. The He-poor SNe are
ordered according to the number of absorption features $N$ present in the
spectra, which is a measure of the degree of line blending. The kinetic energy
per unit mass $E_\mathrm{k}/M_\mathrm{ej}$ is strongly affected by mass at high
velocity and such situations principally occur when the outer density profile
of the ejecta is shallow, leading to the blending of lines. Using the results,
the existing SE-SN taxonomic scheme is adapted. He-rich SNe are split into four
groups, IIb, IIb(I), Ib(II), and Ib, which represent H-rich to H-poor SNe. The
SNe Ic category of broad-lined Ic (Ic-BL) is abandoned in favour of quantifying
the line blending via $\left<N\right>$ before peak. To better reflect the
physical parameters of the explosions, the velocity of Si II at peak and the
half-luminosity decay time $t_{+1/2}$ are included to give SNe Ic a designation
of Ic-$\left<N\right>\left(v_\mathrm{p,SiII}/t_{+1/2}\right)$.
