The Carnegie Supernova Project I: analysis of stripped-envelope supernova light curves

Abstract

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. 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. We found a tentative correlation between the peak absolute $B$-band magnitude and $\hat{I}”m_{15}(B)$, as well as a correlation between the late-time linear slope and $\hat{I}”m_{15}$. Making use of the full set of optical and near-IR photometry, combined with robust host-galaxy extinction corrections, bolometric light curves are constructed and compared to both analytic and hydrodynamical models. 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 $\hat{I}º=0.07$ 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. The inferred ejecta masses are compatible with intermediate mass ($M_{ZAMS}\le 20$ $M_{\odot }$) progenitor stars in binary systems for the majority of SE SNe. Furthermore, the majority of our SNe is affected by significant mixing of ${}^{56}$Ni, particularly in the case of SNe Ic.

46 pages, 25 figures, resubmitted to Astronomy and Astrophysics. The abstract was abridged to fit the allowed arxiv limits