determined from the combination of the intensity of the \[\] emission feature near 5200 Å and the requirement that the energy emitted in the radioactive decay chain of $^{56}$Ni excites other ions and reproduces the observed emission in other lines. This is a slightly larger value than what was derived for SN 1993J [see @Swartz93 and references therein], but it is still fairly typical for core-collapse SNe.

The total mass enclosed within the outer velocity of 4300 [km s$^{-1}$]{} is [$\sim\!\!$ ]{}1.15 [M$_\sun$]{}. Interestingly, our models of [SN 2001ig]{} are quite similar to that of the SN Ic 1994I which underwent significant mass loss, most likely in a binary interaction, and which also ejected [$\sim\!\!$ ]{}1 [M$_\sun$]{} of material [@Sauer06]. @Nomoto94 showed the progenitor star of SN 1994I to be [$\sim\!\!$ ]{}15 [M$_\sun$]{} initially, which suggests that the progenitor of [SN 2001ig]{} was also initially [$\sim\!\!$ ]{}15 [M$_\sun$]{}.

Furthermore, @VanDyk02 and @Maund04 found that both the companion and the progenitor of SN 1993J had intial masses of [$\sim\!\!$ ]{}15 [M$_\sun$]{} and that the companion of SN 1993J is currently 22 [M$_\sun$]{}. @Ryder06 discovered that the companion of [SN 2001ig]{} is currently 10–18 [M$_\sun$]{}, so it seems likely that the progenitors 