  This work explores the detailed chemistry of the Milky Way bulge using the
HERMES spectrograph on the Anglo-Australian Telescope. Here we present the
abundance ratios of 13 elements for 832 red giant branch and clump stars along
the minor bulge axis at latitudes $b=-10^{\circ}, -7.5$ and $-5^{\circ}$. Our
results show that none of the abundance ratios vary significantly with
latitude. We also observe {\color{red}disk-like} [Na/Fe] abundance ratios,
which indicates the bulge does not contain helium-enhanced populations as
observed in some globular clusters. Helium enhancement is therefore not the
likely explanation for the double red-clump observed in the bulge. We confirm
that bulge stars mostly follow abundance trends observed in the disk. However,
this similarity is not confirmed across for all elements and metallicity
regimes. The more metal-poor bulge population at [Fe/H] $\lesssim -0.8$ is
enhanced in the elements associated with core collapse supernovae (SNeII). In
addition, the [La/Eu] abundance ratio suggests higher $r$-process contribution,
and likely higher star formation in the bulge compared to the disk. This
highlights the complex evolution in the bulge, which should be investigated
further, both in terms of modelling; and with additional observations of the
inner Galaxy.
