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Medium resolution (R=4,000 to 9,000) spectra of the near infrared Ca II lines(at 8498, 8542, and 8662 A) in M31 globular cluster integrated light spectraare presented. In individual stars the Ca II triplet (CaT) traces stellarmetallicity; this paper compares integrated CaT strengths to well determined,high precision [Fe/H] values from high resolution integrated light spectra. Thetarget globular clusters cover a wide range in metallicity (from [Fe/H] = -2.1to -0.2). While most are older than 10 Gyr, some may be of intermediate age(2-6 Gyr). A handful (3-6) have detailed abundances (e.g. low [Ca/Fe]) thatindicate they may have been accreted from dwarf galaxies. Using variousmeasurements and definitions of CaT strength, it is confirmed that for GCs with[Fe/H] < -0.4 and older than 2 Gyr the integrated CaT traces cluster [Fe/H] towithin about 0.2 dex, independent of age. CaT lines in metal rich GCs are verysensitive to nearby atomic lines (and TiO molecular lines in the most metalrich GCs), largely due to line blanketing in continuum regions. The [Ca/Fe]ratio has a mild effect on the integrated CaT strength in metal poor GCs. Theintegrated CaT can therefore be safely used to determine rough metallicitiesfor distant, unresolved clusters, provided that attention is paid to the limitsof the measurement techniques.

The Integrated Calcium II Triplet as a Metallicity Indicator: Comparisons with High Resolution [Fe/H] in M31 Globular Clusters