  This paper presents [Fe/H] ratios for GCs in the outer halo of the Andromeda
Galaxy, M31, based on moderate-resolution, integrated light (IL) spectroscopy
of the calcium-II triplet (CaT) lines. The CaT strengths are measured by
fitting Voigt profiles to the lines and integrating those profiles;
integrations of defined bandpasses are also considered. The [Fe/H] ratios are
determined using an empirical calibration with CaT line strength, as derived
from another sample of M31 GCs that were previously studied at high-resolution.
The [Fe/H] ratios for the new GCs reveal that the outer halo GCs are indeed
generally more metal-poor than typical inner halo GCs, though there are several
more metal-rich GCs that look to have been accreted from dwarf satellites. The
metallicities of these GCs also place important constraints on the nature of
the substructure in the outer halo and the dwarf satellites that created this
substructure.
