  Stripped-envelope supernovae (SESNe) are a subclass of core-collapse
supernovae that are deficient in hydrogen (SN~IIb, SN~Ib) and possibly helium
(SN~Ic) in their spectra. Their progenitors are likely stripped of this
material through a combination of stellar winds and interactions with a close
binary companion, but the exact ejecta mass ranges covered by each subtype and
how it relates to the zero-age main-sequence progenitor mass is still unclear.
Using a combination of semi-analytic modeling and numerical simulations, we
discuss how the properties of SESN progenitors can be constrained through
different phases of the bolometric light curve. We find that the light curve
rise time is strongly impacted by the strength of radioactive nickel mixing and
treatment of helium recombination. These can vary between events and are often
not accounted for in simpler modeling approaches, leading to large
uncertainties in ejecta masses inferred from the rise. Motivated by this, we
focus on the late time slope, which is determined by gamma-ray leakage. We
calibrate the relationship between ejecta mass, explosion energy, and gamma-ray
escape time $T_0$ using a suite of numerical models. Application of the fitting
function we provide to bolometric light curves of SESNe should result in ejecta
masses with approximately 20\% uncertainty. With large samples of SESNe coming
from current and upcoming surveys, our methods can be utilized to better
understand the diversity and origin of the progenitor stars.
