The Detailed Chemical Properties of M31 Star Clusters I. Fe, Alpha and
  Light Elements
  We present ages, [Fe/H] and abundances of the alpha elements Ca I, Si I, Ti
I, Ti II, and light elements Mg I, Na I, and Al I for 31 globular clusters in
M31, which were obtained from high resolution, high signal-to-noise ratio
(SNR$>60$) echelle spectra of their integrated light. All abundances and ages
are obtained using our original technique for high resolution integrated light
abundance analysis of globular clusters. This sample provides a never before
seen picture of the chemical history of M31. The globular clusters are
dispersed throughout the inner and outer halo, from 2.5 kpc $<$ R$_{\rm M31}$
$<$ 117 kpc. We find a range of [Fe/H] within 20 kpc of the center of M31, and
a constant [Fe/H]$\sim-1.6$ for the outer halo clusters. We find evidence for
at least one massive globular cluster in M31 with an age between 1 and 5 Gyr.
The alpha-element ratios are generally similar to Milky Way globular cluster
and field star ratios. We also find chemical evidence for a late-time accretion
origin for at least one cluster, which has a different abundance pattern than
other clusters at similar metallicity. We find evidence for star-to-star
abundance variations in Mg, Na, and Al in the globular clusters in our sample,
and find correlations of Ca, Mg, Na, and possibly Al abundance ratios with
cluster luminosity and velocity dispersion, which can potentially be used to
constrain globular cluster self-enrichment scenarios. Data presented here were
obtained with the HIRES echelle spectrograph on the Keck I Telescope.
