emission. Most of the emission lines are forbidden, but some permitted transitions (e.g., the near-IR triplet) are also active. The code is based on the original description by @Axelrod80. The propagation of the $\gamma$-rays is followed with a Monte Carlo procedure [@Cappellaro97]. Level populations are computed assuming non-local thermodynamic equilibrium (non-LTE). A more detailed description is provided by @Mazzali07:02ap.

Modeling the spectra also requires knowledge of the reddening of, and distance to, the SN. As discussed in §\[ss:early\], the reddening within is negligible and we have only an upper limit from our data, so we adopt a total reddening of $E\left(B-V\right)=0.011$ mag from @Schlegel98 for the models. For the distance to [SN 2001ig]{}we have used a recession velocity of 939 [km s$^{-1}$]{}[$z=0.003132$; @Koribalski04] throughout this paper, yielding a distance modulus of $m-M=30.5$ mag with $H_0 = 73$ [km s$^{-1}$]{} [Mpc$^{-1}$]{} [@Riess05], assuming the entire recession velocity is due to the Hubble flow. However, there is some uncertainty in this value due to the relatively small distance to . A search of the literature reveals a range in distance moduli for this galaxy of 30.2–30.7 mag using various independent techniques [HyperLEDA[^3]; @Tully88; @Mould00; @Meurer06; @Davis09 private communication[^4]]. The value of 30.5 