Progenitors of Long-Duration Gamma-ray Bursts
  We review the current scenario of long-duration Gamma-ray burst (LGRB)
progenitors, and in addition, present models of massive stars for a mass range
of $10\text{--}150 \, \mathrm{M}_\odot$ with $\Delta \mathrm{M}=10 \,
\mathrm{M}_\odot$ and rotation rate $v/v_{\rm{crit}}=0$ to $0.6$ with a
velocity resolution $\Delta v/v_{\rm{crit}} =0.1$. We further discuss possible
metallicity and rotation rate distribution from our models that might be
preferable for the creation of successful LGRB candidates given the observed
LGRB rates and their metallicity evolution. In the current understanding, LGRBs
are associated with Type-Ic supernovae (SNe). To establish LGRB-SN correlation,
we discuss three observational paths: (i) space-time coincidence, (ii) evidence
from photometric light curves of LGRB afterglows and SN Type-Ic, (iii)
spectroscopic study of both LGRB afterglow and SN. Superluminous SNe are also
believed to have the same origin as LGRBs. Therefore, we discuss constraints on
the progenitor parameters that can possibly dissociate these two events from a
theoretical perspective. We further discuss the scenario of single star versus
binary star as a more probable pathway to create LGRBs. Given the limited
parameter space in the mass, mass ratio and separation between the two
components in a binary, binary channel is less likely to create LGRBs to match
the observed LGRB rate. Despite effectively-single massive stars are fewer in
number compared to interacting binaries, their chemically homogeneous evolution
(CHE) might be the major channel for LGRB production.
