can quench the ejected material and produce a low luminosity SN. Stars with masses above 25$M_\odot$, formed in metal-poor or slightly sub-solar metallicity regions can produce low-luminosity, BH-forming Type IIP SNe. Type IIL/b events can be produced through this process from stars having masses $\textgreater~ 25$ and generated in regions with solar (or super-solar) metallicity. So, the metallicity information at the SN location and the estimation of the initial mass are essential to constrain the triggering mechanisms of these explosions.

SN 2008in was discovered in the nearby galaxy M 61 (NGC 4303). The first unfiltered CCD images of  were taken by Koichi Itagaki on 2008 December 26.79 (all times in UT hereafter) and 27.69 at a magnitude of 14.9. Independent observations of this event by K. Kadota showed the transient at an unfiltered mag of 15.1, In addition W. Wells recorded the SN on 2008 December 28.46 at $V$ and $R$ band magnitudes of 14.3 and 13.2, respectively [@nakano08]. Low and mid-resolution spectroscopic observations indicate an early discovery for SN 2008in (within 1$-$2 weeks after core-collapse). The spectra showed highly blueshifted H$_\alpha$ and H$_\beta$ absorptions (by $\sim$ 9000 ) with weaker emission components [@chakraborti08; @foley08; @stritzinger08]. The presence of prominent 