negligible continuum and are marked by pronounced emissions of forbidden lines [\[\]]{} $\lambda\lambda$7291, 7323, and fading of the absorption features of hydrogen and metallic lines.

In Figure \[fig:spec\_ccsne\], we compare the +99d spectrum of  with the spectra of other Type IIP SNe observed at similar phases that is at roughly the time when the light curve changes from the photospheric plateau to the nebular phase. The phases quoted for each event are with reference to the moment of inflection ($ti$; see Figure \[fig:rotse\]). The narrow P-Cygni  profile and the presence of strong lines of  at $\lambda$6142 and $\lambda$6497 of  show striking resemblance to the low-luminosity SNe 1997D, 1999br, 1999eu, 2001dc and 2005cs. On the other hand, the normal Type IIP SNe 2004et, 2008gz show broader profiles of  and weaker lines of . It is noted that in the blue wing of  more metallic lines get resolved than that in the normal IIP SNe and this arises due to smaller line widths of hydrogen lines seen in low-luminosity IIP SNe (@fraser10 and references therein). In addition, the  line in the low-luminosity SNe show stronger absorption components due to lower ejecta temperature than that in the normal luminosity Type IIP SNe 2004et 