  In a recent paper we calculated the field equations of spin-3/2 fields in a
$D$-dimensional Reissner-Nordstr\"om black hole spacetime whilst maintaining
the gauge symmetry of the Rarita-Schwinger equation. We were also able to
determine the quasi-normal modes of the associated gauge invariant variables
using the WKB approximation and the asymptotic iteration method (AIM). However,
it was found that for higher dimension, and especially for the near extremal
cases, the effective potential developed another maximum. The shape of the
potential posed difficulties for the WKB approximations, as well as the AIM. As
such, in this proceedings we would like to explore the connection between the
AIM and the continued fraction method, and determine a possible reason for the
difficulty in calculating the quasi-normal modes for spin-3/2 fields in this
spacetime.
