profile with a complex top and does not seem to exhibit the same double-peaked nature of the \[\] emission. This differs from the results of @Foley03 for the energetic broad-lined SN Ic 2002ap, which showed identical \[\] and \] profiles. In addition, the flux in the \] line appears to be more centrally concentrated in [SN 2001ig]{} compared to SN 2002ap.

It has been proposed that the double-peaked \[\] profile of SN 2005bf was caused by a unipolar blob or jet [@Maeda07] while its polarization signature was attributed to a possible “tilted jet” passing through an asymmetric photosphere [@Maund07b; @Maund07]. Both our models of late-time spectra of [SN 2001ig]{} and the similarity of the profiles in our late-time spectra to those of SN 1993J [@Matheson00] indicate clumpy, oxygen-rich ejecta as well (see §\[s:model\] for more information regarding the models and ejecta). Thus, [SN 2001ig]{} probably has large-scale asymmetry in its ejected oxygen, either in the form of a blob or jet (tilted or otherwise), while the distributions of magnesium and calcium appear more uniform (though the magnesium seems only marginally more uniform than the oxygen). This is supported by @Fransson89, who predicted that magnesium and calcium should be found closer 