wavelength shifts were then applied to the LRIS data after cross-correlating a template sky to the night-sky lines that were extracted with the SN. Using our own IDL routines, we fit spectrophotometric standard-star spectra to the LRIS data in order to flux calibrate our spectra and to remove telluric lines [@Wade88; @Matheson00].

Each EMMI observation was reduced independently and the final spectra were combined with a pixel-rejection algorithm based on the mean.

Spectral Analysis {#s:analysis}
=================

Early-Time Spectra {#ss:early}
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We present our early-time spectra of [SN 2001ig]{} in Figure \[f:early\_spec\]; all have had the recession velocity of removed [939 [km s$^{-1}$]{}, from @Koribalski04]. The first spectrum of [SN 2001ig]{}, taken on 2001 Dec. 11 (8 days past explosion), shows only a few strong, broad absorption features. We conjecture that the feature near 4000 Å is [H$\gamma$]{} and the feature near 4300 Å is a blend of lines (near a rest wavelength of 4570 Å) blueshifted by [$\sim\!\!$ ]{}22,500 [km s$^{-1}$]{} and [$\sim\!\!$ ]{}18,200 [km s$^{-1}$]{}, respectively. Unfortunately, this identification is somewhat dubious since the [H$\gamma$]{}feature appears to be unusually strong.

Instead, we note that this pair of features resembles the “W” feature seen in very early-time spectra of the 