variety of star formation histories [@b35; @b36; @b37] that are predicted to lead to variations in their metallicity distribution functions and chemical abundances. It has also been suggested these variations could be attributed to differences in the IMFs of these galaxies [@b73]. If the IMFs are the root cause of these differences then this would also lead to differences in the age-metallicity relationship, which is observed by both [@b32] and [@b34]. From observations, field stars in dwarf galaxies do exhibit different abundance ratios from Milky Way (MW) field stars, e.g., lower \[$\alpha$/Fe\] ratios and variations in neutron capture element ratios at intermediate metallicities these typically do not show up until \[Fe/H\] $\sim -1.5$ [@b86; @b87; @b13; @b27; @b41; @b42; @b28]. At metallicities below \[Fe/H\] $= -1.5$ the abundance variations between field and GC stars become less pronounced in dwarfs and the MW [@b68; @b81; @b83; @b45]; a good example of this is M54, located at the heart of the Sagittarius (Sgr) dwarf accretion remnant. M54 has a much lower metallicity than the Sgr field stars (e.g., @b83) and the \[$\alpha$/Fe\] ratios resemble the field stars in the MW halo and its detailed chemical abundance ratios resemble the patterns seen in 