2005cs [@pastorello04; @pastorello09], 2008bk [@vandyk11] and 2009md [@fraser10]. These events have explosion energy ($\sim 10^{50}$ erg) and ejected $^{56}$Ni-mass ($2-7\times10^{-3}$ ), both lower by a factor of 10 than normal, and low expansion velocity $\sim$1000 (@pastorello09 and references therein). The low-luminosity IIP SNe are debated because of the unknown nature of their progenitors. The first reported faint SN was SN 1997D [@turatto98; @benetti01], and the observed properties of its light curves and spectra were explained in terms of significant fallback of ejected material on a newly formed black hole (BH), created through the core collapse of a massive progenitor ($M \ga 20M_\odot$, @zampieri98 [@zampieri03]). Alternatively, SN 1997D was interpreted as the explosion of a less massive progenitor ($8-12M_\odot$, @chugai00), close in mass to the lower limit for stars that can undergo core-collapse. @heger03 suggested that low-luminosity Type IIP events are electron capture SNe produced by low-mass progenitors giving rise to ONeMg cores. This is further supported through investigations of pre-explosion images [@maund05a; @maund05b], though @eldridge07 have ruled out the possibility of such a mechanism for the low-luminosity SN 2005cs. According to the formalism of @heger03 and @eldridge04, no star having initial mass less than 22 can form a BH, which 