13 giants and the comparison star HD 141531 using the same lines presented in Y05. These measurements were performed to ensure that the abundances would be on the same scale as the NGC 6752 giants studied in Y05. Zr was chosen because we compare the Rb and Zr abundances to look for a large ratio \[Rb/Zr\] as well as a detectable dispersion, i.e., the hallmark of a high neutron-density environment and the possible signature of pollution from IM-AGBs. Al, Si, and Y were also chosen because Y05 found evidence for correlations between Al and Si, Al and Y, and Al and Zr in NGC 6752. While our sample size in M 13 is small, it would be interesting to see if similar correlations are present. La and Eu were measured since these neutron-capture elements offer an insight into the ratio of $s$-process to $r$-process material. Furthermore, the ratio \[Pb/La\] has been used to test predictions from AGB models. In Table \[tab:abund\] we present our measured elemental abundances for Al, Si, Rb, Y, Zr, La, Eu, and Pb in the program stars. The adopted solar abundances for Al, Si, Y, Zr, La, and Eu were 6.47, 7.55, 2.24, 2.60, 1.13, and 