to be $\sim$100 K for both standard stars, and this is adopted for the five science targets given the similarity in S/N and $\mathrm{T}_{\mathrm{eff}}$ in our sample.

The $\Delta$$v_t$ is found by allowing the slope log$\epsilon$(Fe I) vs. reduced EW to vary such that the range of log$\epsilon$([Fe$\;$[Roman[1]{}]{}]{}) values span 1 $\sigma$ over the range of reduced EWs, similar to the method used to find $\Delta\mathrm{T}_{\mathrm{eff}}$. The $\Delta$$v_t = 0.2$ $\mathrm{kms^{-1}}$ for both standard stars and is adopted for the five science targets.

Physical gravities are adopted from the IRFM, thus log(g) depends on the distance to the star (or cluster), reddening, $\mathrm{T}_{\mathrm{eff}}$ value, turn-off mass, and photometry; an estimate in the uncertainty of log(g) is calculated by quantifying and propagating the errors in these parameters. After calculating log(g) and varying these parameters by the errors described in this Section, $\Delta$log(g) = 0.2 dex (Assuming no covariance).

Comparison of Stellar Parameters and Iron with the Standard Stars {#sec:Fecomp}
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To test the validity of this abundance analysis technique the procedure is applied to the standard stars in M3 and M13 using the model atmospheres and EWs of this work and comparing the [Fe$\;$[Roman[1]{}]{}]{} abundance with CM05. The model atmosphere parameters 