  The two peculiar Type Ic supernovae (SNe) 1997ef and 1997dq are shown to have
very similar photometric and spectral evolution in the epochs when both SNe are
observed (i.e. beyond $\sim 80$ days after the explosion). The early light
curves and spectra of SN 1997ef suggested that this was a ``hypernova,'' or
``SN 1998bw-like Type Ic supernova.'' The fact that the two SNe are very
similar allows us to extend the time coverage of this type of event, since SN
1997dq, unlike SN 1997ef, was observed well into the nebular phase. In contrast
to SN 1998bw, the spectra of these two SNe did not become fully nebular until
almost one year after the explosion. During a long transition phase, lasting at
least 6 months, the SNe developed nebular emission in lines of [\OI] and
[\CaII], but at the same time they retained an underlying, photospheric-type
spectrum, originating at very low velocities. Spectral synthesis techniques are
used to model the spectrum of SN 1997dq, suggesting that it produced $\sim 0.16
\Msun$ of \Nifs, and that a significant fraction of this is located in a dense,
low-velocity inner region.
