  Based upon a metallicity selection, we identify a significant sub-population
of the inner halo globular clusters in the Andromeda Galaxy which we name the
Dulais Structure. It is distinguished as a co-rotating group of 10-20 globular
clusters which appear to be kinematically distinct from, and on average more
metal-poor than, the majority of the inner halo population. Intriguingly, the
orbital axis of this Dulais Structure is closely aligned with that of the
younger accretion event recently identified using a sub-population of globular
clusters in the outer halo of Andromeda, and this is strongly suggestive of a
causal relationship between the two. If this connection is confirmed, a natural
explanation for the kinematics of the globular clusters in the Dulais Structure
is that they trace the accretion of a substantial progenitor (~10^11 Msun) into
the halo of Andromeda during the last few billion years, that may have occurred
as part of a larger group infall.
