& 0.06 & 0.18\
[O$\;$[Roman[1]{}]{}]{} &-0.18 & 0.00 &-0.01 & 0.18\
[Mg$\;$[Roman[1]{}]{}]{} &-0.13 &-0.01 &-0.02 & 0.14\
[Al$\;$[Roman[1]{}]{}]{} &-0.11 &-0.01 &-0.04 & 0.12\
[Si$\;$[Roman[1]{}]{}]{} &-0.12 &-0.03 &-0.03 & 0.12\
[Ca$\;$[Roman[1]{}]{}]{} &-0.19 &-0.10 &-0.14 & 0.26\
[Ti$\;$[Roman[1]{}]{}]{} &-0.20 &-0.05 &-0.05 & 0.21\

Standard Star Comparison {#sec:CMcomp}
------------------------

The standard star abundances are compared to CM05 in detail here. The EWs and stellar parameters between this work and CM05 are in good agreement, as summarized in Sections \[sec:EWcomp\] and \[sec:Fecomp\]; thus the remaining elemental abundances are now compared. The standard star abundances are shown in Table \[table:CohenComp\] ; the average abundance difference ($\pm \sigma$) between this work and CM05 is 0.08 $\pm$ 0.13 and 0.14 $\pm$ 0.11 for M3-C41303-2217 and M13-III-18 respectively which we consider good agreement. In the case where there are derived abundances for both the neutral and ionized species (except for the case of Fe), the weighted mean and error between the two is reported and compared with CM05. As opposed to the other elemental abundances, oxygen was determined with respect to [Fe$\;$[Roman[2]{}]{}]{} in order to keep consistent with CM05.

For the M3 star most of the elements agree within the errors with the exception of Sc, V, Ni, 