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The equation found for Single Mercury fit for both Peaks and Dips in Figure 8 is as follows:

\begin{equation} \begin{split}\displaystyle E_{n}[eV](fit)&\displaystyle=(0.136\pm 0.03)n+(4.35\pm 0.16)\\ E_{a}[eV](fit)&\displaystyle=(0.136\pm 0.04)(0.5)+(4.35\pm 0.16)\\ \displaystyle E_{a}[eV](fit)&\displaystyle=4.42\pm 0.20\end{split}\\ \end{equation}

Using the above equation, the intercept was found to be a value of \(E_{a}=4.418\pm 0.20\textrm{eV}\) at \(n=0.5\). This value does not match the accepted values of \(4.6674eV\) and \(4.8865eV\) (NIST database values) within uncertainty. The method used in the analysis of Figure 7 had much more accurate results, thus it was concluded that although the value of \(n=2\) is not on the line of best fit, using separate linear fits to approximate \(\Delta E\) versus \(n\) is a better method.