  We present the final results of an imaging and spectroscopic search for stars
in the Large Magellanic Cloud (LMC) with C II 7231, 7236 emission lines. The
goal is to identify and study [WC11] stars, the coolest of the low-mass
Wolf-Rayet sequence, and a subset of central stars of planetary nebulae where
the C II lines are known to be especially prominent. A recent serendipitous
discovery of an LMC [WC11] raised the possibility that these objects, although
difficult to identify, might in fact be more common than previously believed.
Several new members of this rare class have been found in this survey. It now
seems clear, however, that a significant number of these stars are not hiding
amongst the general [WC] population. We point out that the C II doublet
intensity ratio observed in our spectra proves to neatly divide the objects
into two distinct groups, with the C II emission likely originating from either
the stellar wind or a surrounding nebula. The physics of the C II emission
mechanism correctly explains this bifurcation. Spectral subtypes are suggested
for most of the objects. The numerous spectroscopic clues now available for
these objects should facilitate future detailed modeling.
