Stripped-envelope ( SE ) supernovae ( SNe ) include H-poor ( Type IIb ) , H-free ( Type Ib ) and He-free ( Type Ic ) events thought to be associated with the deaths of massive stars .
The exact nature of their progenitors is a matter of debate with several lines of evidence pointing towards intermediate mass ( M _ { init } < 20 \leavevmode \nobreak M _ { \odot } ) stars in binary systems , while in other cases they may be linked to single massive Wolf-Rayet stars .
Here we present the analysis of the light curves of 34 SE SNe published by the Carnegie Supernova Project ( CSP-I ) , which are unparalleled in terms of photometric accuracy and wavelength range .
Light-curve parameters are estimated through the fits of an analytical function and trends are searched for among the resulting fit parameters .
Detailed inspection of the dataset suggests a tentative correlation between the peak absolute B -band magnitude and \Delta m _ { 15 } ( B ) , while the post maximum light curves reveals a correlation between the late-time linear slope and \Delta m _ { 15 } .
Making use of the full set of optical and near-IR photometry , combined with robust host-galaxy extinction corrections , comprehensive bolometric light curves are constructed and compared to both analytic and hydrodynamical models .
This analysis finds consistent results among the two different modeling techniques and from the hydrodynamical models we obtained ejecta masses of 1.1 - 6.2 M _ { \odot } , ^ { 56 } Ni masses of 0.03 - 0.35 M _ { \odot } , and explosion energies ( excluding two SNe Ic-BL ) of 0.25 - 3.0 \times 10 ^ { 51 } erg .
Our analysis indicates that adopting \kappa = 0.07 cm ^ { 2 } g ^ { -1 } as the mean opacity serves to be a suitable assumption when comparing Arnett-model results to those obtained from hydrodynamical calculations .
We also find that adopting He i and O i line velocities to infer the expansion velocity in He-rich and He-poor SNe , respectively , provides ejecta masses relatively similar to those obtained by using the Fe ii line velocities , although the use of Fe ii as a diagnostic does imply higher explosion energies .
The inferred range of ejecta masses are compatible with intermediate mass ( M _ { ZAMS } \leq 20 M _ { \sun } ) progenitor stars in binary systems for the majority of SE SNe .
Furthermore , our hydrodynamical modeling of the bolometric light curves suggest a significant fraction of the sample may have experienced significant mixing of ^ { 56 } Ni , particularly in the case of SNe Ic .