  We present outburst and quiescence spectra of the classical nova KT Eri and
discuss the appearance of a sharp HeII 4686 Ang emission line, whose origin is
a matter of discussion for those novae that showed a similar component. We
suggest that the sharp HeII line, when it first appeared toward the end of the
outburst optically thick phase, comes from the wrist of the dumbbell structure
characterizing the ejecta as modeled by Ribeiro et al. (2013). When the ejecta
turned optically thin, the already sharp HeII line became two times narrower
and originated from the exposed central binary. During the optically thin
phase, the HeII line displayed a large change in radial velocity that had no
counterpart in the Balmer lines (both their narrow cores and the broad
pedestals). The large variability in radial velocity of the HeII line continued
well into quiescence, and it remains the strongest emission line observed over
the whole optical range.
