and 2008gz [@turatto98]. In Figure \[fig:line\_id\], we have identified the spectral features in a late-plateau phase (+99d) spectrum which covers the full wavelength range from 0.4 to 0.95 . For line identification we have followed @pastorello04, where different spectral lines were identified for the +102d spectrum of a low-luminosity SN 1999br. We are able to identify all the features and the spectral profiles of all the elements are similar to the archetypal low-luminosity IIP SNe 1997D, 2005cs and 1999br (@pastorello04 and references therein).

![image](line_id.ps){width="15cm"}

![image](velocity_all.ps){width="15cm"}

Figure \[fig:vel\_line\] shows the spectral evolution of , , D, , , and  lines. In Figure \[fig:vel\_bulk\] (left panel), we show the expansion velocities of the ejecta derived from Balmer and lines. The later is a good indicator of photospheric velocity. The expansion velocities of the H-envelope are estimated using absorption minima of the P-Cygni profiles and at the two earliest phases (+7d and +14d)  and  show a broad P-Cygni profile which, with time, becomes narrower at later phases keeping the position of the emission peak centered near zero velocity. The  line velocity starts at about 7000  at +10d, reaches 4000  at +50d and flattens at a level of 1200  in the nebular phases. It 