note that there is also an increase in the flux in the wings of the \[\] feature near $\pm$2000–5000 [km s$^{-1}$]{}.

The complex structure of the \] $\lambda$4571 and \[\] $\lambda\lambda$6300, 6364 lines has been seen previously in another well-studied Type IIb, SN 1993J [@Matheson00]. They found that the \[\] and \] line profiles resulted from clumps in the ejecta while the \[\] lines did not. They also pointed out that this is consistent with the explosion scenario first proposed for SN 1987A by @Li92 [@Li93], in which the emission from oxygen comes from clumps of newly synthesized material while the calcium emission originates mainly in preexisting uniformly distributed material. @Filippenko89 found similar irregularities in the \[\] $\lambda\lambda$6300, 6364 lines of the SN Ib 1985F. They suggested that the spectral peculiarities come either from Rayleigh-Taylor fingers of higher-speed material or from local density enhancements.

The \[\] doublet of [SN 2001ig]{} somewhat resembles that of the peculiar SN Ib 2005bf [@Modjaz08] in that [SN 2001ig]{}may also show a double-peaked profile with one of the peaks near zero velocity and the other blueshifted by a few thousand [km s$^{-1}$]{}. However, the \] line in [SN 2001ig]{} at all epochs has a broad 