  We discuss the emerging trend that super-Chandrasekhar Type Ia Supernovae
(SCSNe) with progenitor mass estimates significantly exceeding 1.4 M_sun tend
to explode in metal-poor environments. While Taubenberger et al. 2011 noted
that some of the SCSNe host galaxies are relatively metal-poor, we focus
quantitatively on their locations in the hosts to point out that in three out
of four cases, the SCSNe explosions occurred in the outer edge of the disks of
their hosts. It is therefore very likely that their progenitors had far lower
metallicities than those implied by the metallicity of their hosts' central
regions. In two cases (SN 2003fg and SN 2009dc) the explosion sites were
outside 99% of the host's light, and in one case (SN 2006gz) the host's radial
metallicity slope indicates that the explosion site is in a metal-poor region.
The fourth case (SN 2007if) has the lowest spectroscopically measured SN Ia
host metallicity (Childress et al. 2011. It may be possible to explain each of
these unusually bright events through some progenitor scenario specific to that
case, but a much simpler and straightforward conclusion would be to ascribe the
controlling factor to the only physical aspect they have in common --- metal
poor environments.
