two out of four lines that overlap with CM05 and there are $\sim 15 \%$ discrepancies in EW for the common lines; furthermore if \[La/[Fe$\;$[Roman[1]{}]{}]{}\] is calculated using the solar values and [Fe$\;$[Roman[1]{}]{}]{} parameters of CM05 then the La abundances agree.

Overall, the standard star comparison is within good agreement and we consider the methods used both here and with the target stars sound. The target star abundances are discussed in detail in the following section.

\[table:CohenComp\]

[@lccccccr@]{}\
Species[^14] & Abundance &$\sigma$ & N & Abundance &$\sigma$ & N & $\Delta$[^15]\
& &\

[\[]{}[Fe$\;$[Roman[1]{}]{}]{}/H\] &-1.33 &0.05 & 103 &-1.37 &0.05 &126 &0.04\
[\[]{}[Fe$\;$[Roman[2]{}]{}]{}/H\] &-1.33 &0.05 & 14 &-1.34 &0.05 &14 &0.01\
[\[]{}O/Fe\] & 0.49 &0.10 & 2 & 0.33 &0.05 &2 &0.10\
[\[]{}Na/Fe\] &-0.27 &0.05 & 2 &-0.39 &0.09 &3 &0.12\
[\[]{}Mg/Fe\] &0.33 &0.13 & 2 &0.40 &0.11 &3 &-0.07\
[\[]{}Al/Fe\] &0.32 &0.20 & 2 &... &... &... &...\
[\[]{}Si/Fe\] &0.16 &0.08 & 2 &0.20 &0.05 &9 &-0.04\
[\[]{}Ca/Fe\] &0.25 &0.05 & 16 &0.08 &0.05 &15 &0.17\
[\[]{}Sc/Fe\] &-0.01 &0.05 & 3 &0.15 &0.05 &7 &-0.16\
[\[]{}Ti/Fe\] &0.17 &0.05 & 29 &0.10 &0.05 &25 &0.07\
[\[]{}V/Fe\] &0.05 &0.10 & 12 &-0.18 &0.06 &8 &0.23\
[\[]{}Cr/Fe\] &0.08 &0.05 & 7 &0.01 