The identification of SN progenitors has always been a non-trivial task in the transient research arena. While, the pre-explosion HST images of supernova site aid in the direct detection of the progenitor, only a dozen of such cases exist. Hydrodynamical modelling of events can predict the pre-supernova mass, but again the uncertain amount of matter lost through winds renders the estimated main-sequence progenitor mass dubious. The detection of circumstellar interaction at radio and X-ray wavelengths comes to the rescue, but only in a few cases, as observations at these wavelengths are often not available. In this talk, I will discuss the optical signatures in the spectra of supernovae IIP which can be used estimate the pre-supernova mass loss rate and hence the main sequence progenitor masses of supernovae IIP.