at early times [@Phillips01; @Clocchiatti01]. Examples of both at similar ages are plotted for comparison in Figure \[f:early\_spec\] and there do appear to be quite a few similarities among these objects. However, it should be noted that [H$\alpha$]{} (both the absorption and emission components) is weaker in [SN 2001ig]{}. In addition, the overall continuum shape of [SN 2001ig]{} does not change much during this two-week period.

Figure \[f:early\_spec\] also indicates that [SN 2001ig]{}has a bluer continuum than either SN 1987K or SN 1993J; however, this could be due to reddening. Both SNe 1987K and 1993J are plotted with no reddening correction, which is approximately consistent with observations [@Richmond94], but there is also evidence that the color excess of SN 1993J is as high as 0.25–0.32 mag [@Richmond94; @Clocchiatti95].

Transition Spectra {#ss:transition}
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Our spectra from [$\sim\!\!$ ]{}5.5 weeks past explosion to [$\sim\!\!$ ]{}8 weeks past explosion are presented in Figure \[f:mid\_spec\]. The most obvious change in the spectra of [SN 2001ig]{} from Figure \[f:early\_spec\] to Figure \[f:mid\_spec\] is that the flux in the blue part of the continuum has decreased significantly; [SN 2001ig]{} now looks very much like SN 1993J in its overall continuum shape. In addition, SNe 2001ig and 