the  emitting zone along with its depletion by inner metal shells (like ). The broader absorption dip ‘B’ is identified as a blend of  $\lambda$6497, ,  and . An exceptionally strong  lines is quite typical for cooler ejecta of less energetic fain SNe. The segment ‘C’ is speculated to be a footprint of  multiplets as the evolution of its linewidths seems to be correlated with the other  lines. It is noted, however, that in a few normal Type IIP SNe 1999em, 2004et and 2008gz, the spectral feature near ’C’ at early plateau phases was also identified as a signature of high velocity  component, and in the present spectra its presence cannot be completely ruled out.

The evolution of  is similar to the evolution of . The P-Cygni profile of  is clearly visible in the +7d spectrum, and later on, the emission component is blanketed by various metal lines, mainly due to  $\lambda$4924, $\lambda$5018 and $\lambda$5169. Traces of  and   absorption dips indicate that from the beginning of the nebular phase H shells of ejecta and the regions containing  ions move with a comparable velocity, reaching an asymptotic value $\sim$ 1000   nearly 140 days after the explosion. In the +14d spectrum,  lines 