can be seen from the right panel of Figure \[fig:vel\_bulk\] that in the comparable phases, the  line velocities of low-luminosity SNe are less than half those of normal IIP SNe 1999em and 2004et, whereas the  velocities are more like low-luminosity SN 2005cs. To estimate the photospheric velocity of the transient we have computed the velocities of different  lines $\lambda$4924, $\lambda$5018, and $\lambda$5169 at different phases. The first marginal detection of these lines is in the +14d spectrum and they became prominent in later stages of evolution. For , the average velocity of these lines (and hence roughly the photospheric velocity) at +14d is about 4450 , which is comparable with that of low luminosity SNe and much less than ordinary Type IIP events (see Figure 12 of @pastorello09).

![image](velocity_bulk.ps){width="9cm"}![image](velocity_bulkcomp.ps){width="9cm"}

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

The emergence of absorption dips in the blue wings of  is clearly seen in the post +60d spectra [^7] and the absorption dips have been marked with A, B and C in Figure 8. We distinguish ‘A’ as an absorption dip due to  and  and its equivalent width (EW) increases from 12.85 Å at +60d to 19.45 Å at +143d. This progressively stronger absorption dip requires a steep deceleration of 