We present abundances of globular clusters in the Milky Way and Fornax from integrated light spectra .
Our goal is to evaluate the consistency of the integrated light analysis relative to standard abundance analysis for individual stars in those same clusters .
This sample includes an updated analysis of 7 clusters from our previous publications and results for 5 new clusters that expand the metallicity range over which our technique has been tested .
We find that the [ Fe/H ] measured from integrated light spectra agrees to \sim 0.1 dex for globular clusters with metallicities as high as [ Fe/H ] = -0.3 , but the abundances measured for more metal rich clusters may be underestimated .
In addition we systematically evaluate the accuracy of abundance ratios , [ X/Fe ] , for Na I , Mg I , Al I , Si I , Ca I , Ti I , Ti II , Sc II , V I , Cr I , Mn I , Co I , Ni I , Cu I , Y II , Zr I , Ba II , La II , Nd II , and Eu II .
The elements for which the integrated light analysis gives results that are most similar to analysis of individual stellar spectra are Fe I , Ca I , Si I , Ni I , and Ba II .
The elements that show the greatest differences include Mg I and Zr I .
Some elements show good agreement only over a limited range in metallicity .
More stellar abundance data in these clusters would enable more complete evaluation of the integrated light results for other important elements .