with possible absorption due to [H$\gamma$]{}  and , respectively.

The feature near 4600 Å is most likely [H$\beta$]{}  while the noisy dips just below 4800 Å are probably due to a combination of $\lambda\lambda$4921, 5015 and $\lambda\lambda$4924, 5018. Also seen is weak absorption likely due to $\lambda$5169 near 5030 Å  and quite broad, weak absorption from the near-infrared (IR) triplet around 8150 Å. On 2001 Dec. 23, we acquired the fifth spectrum from the top of Figure \[f:early\_spec\]. Again, we detect the [H$\alpha$]{} P-Cygni line, although now it has a far more complex profile with a larger full width at half-maximum intensity (FWHM) than previously seen. This implies that the [H$\alpha$]{} feature is now likely becoming blended with $\lambda$6355. The feature near 5600 Å in this spectrum clearly shows two local minima which are probably due to $\lambda$5876 and  D. Also in this observation we detect distinct [H$\beta$]{}, $\lambda$4921, and $\lambda$5015 absorption, in addition to absorption from the near-IR triplet around 8200 Å. Finally, extremely strong absorption due to  H&K can now be seen near 3750 Å. It has been pointed out that in many ways the first few spectra of [SN 2001ig]{} resemble those of SNe 1987K and 1993J 