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Measurements of [Fe/H] and [$\alpha$/Fe] can probe the minor merging historyof a galaxy, providing a direct way to test the hierarchical assembly paradigm.While measurements of [$\alpha$/Fe] have been made in the stellar halo of theMilky Way, little is known about detailed chemical abundances in the stellarhalo of M31. To make progress with existing telescopes, we apply spectralsynthesis to low-resolution DEIMOS spectroscopy (R $\sim$ 2500 at 7000Angstroms) across a wide spectral range (4500 Angstroms $<$ $\lambda$ $<$ 9100Angstroms). By applying our technique to low-resolution spectra of 170 giantstars in 5 MW globular clusters, we demonstrate that our technique reproducesprevious measurements from higher resolution spectroscopy. Based on theintrinsic dispersion in [Fe/H] and [$\alpha$/Fe] of individual stars in ourcombined cluster sample, we estimate systematic uncertainties of $\sim$0.11 dexand $\sim$0.09 dex in [Fe/H] and [$\alpha$/Fe], respectively. We apply ourmethod to deep, low-resolution spectra of 11 red giant branch stars in thesmooth halo of M31, resulting in higher signal-to-noise per spectral resolutionelement compared to DEIMOS medium-resolution spectroscopy, given the sameexposure time and conditions. We find $\langle$[$\alpha$/Fe]$\rangle$ = 0.49$\pm$ 0.29 dex and $\langle$[Fe/H]$\rangle$ = 1.59 $\pm$ 0.56 dex for oursample. This implies that---much like the Milky Way---the smooth halo of M31 islikely composed of disrupted dwarf galaxies with truncated star formationhistories that were accreted early in the halo's formation.

Elemental Abundances in M31: Alpha and Iron Element Abundances from Low-Resolution Resolved Stellar Spectroscopy in the Stellar Halo