spherical distribution of  in the SN ejecta. In the three high S/N spectra labeled with +54d, +60d and +87d, a tiny absorption dip overlaid on the emission component of the  D P-Cygni is seen and since these spectra are redshift corrected, these dips are impressions of intervening interstellar matter present in the host galaxy. The absence of any similar absorption dip in the blue wing of the D profile, expected from the Galactic interstellar matter, confirms that there is little absorption from the Milky Way in the line of sight of .

The spectral evolution of  $\lambda$6248 and the s-process element  $\lambda$6142 is clearly seen in . In the +7d and +14d spectra, there is no clear evidence for the presence of these two elements; however in the +54d spectrum they are prominent. The absorption components become stronger with time and persist until the +143d spectrum. In contrast, in the normal Type IIP SNe 2004et [@sahu06], 1999em [@elmhamdi03a] and 2008gz [@roy11] these features disappeared at $\sim$ 170 day after the explosion. The ejecta of underluminous Type IIP SNe expand at a lower velocity than those of normal ones. So, the Ba lines in low luminosity events persist for a longer 