  In the standard holographic ``dictionary'', the deep infrared of the strongly
coupled boundary field theory is studied by examining the bulk region near to
the event horizon of a simple AdS-Reissner-Nordstr\"{o}m black hole, near to
extremality. Recently Horowitz et al. have argued that this is not correct,
\emph{except} in the case of small toroidal black holes, which are therefore
revealed to be particularly interesting and important. On the other hand, the
Weak Gravity Conjecture postulates that black holes (including toroidal black
holes) which are extremely near to extremality spontaneously emit black holes
of the same kind. We show that, in the toroidal case, these ``emitted'' black
holes are always small in the sense of Horowitz et al. As an application, we
discuss the Grinberg-Maldacena analysis of the way one-point functions,
evaluated outside an AdS-Reissner-Nordstr\"{o}m black hole, depend on the
proper time of fall from the event horizon to the Cauchy horizon. We find that,
for emitted toroidal black holes, this dependence effectively drops out.
