and La (which lie within 2 $\sigma$ of each other), of Ca (3 $\sigma$), and of Zn (4 $\sigma$). [@b12] find Sc to be -0.11 dex lower than CM05 and we find also find Sc to be lower (by -0.16 dex). The V abundance in this work has only 3 overlapping lines with CM05, all with different log(gf) values ($\sim$0.05 dex difference). The Ni abundances in this work are derived with log(gf) values that are quite different than CM05, with all 8 of the overlapping lines showing differences up to 0.24 dex. La is derived from 2 lines in this work with similar EWs and log(gf) values to CM05, and from one additional La line; after taking into account the differences in adopted solar values between this work and CM05 the La abundances agree within the errors. The M3 Ca abundance derived by [@b12] differs from CM05 by -0.13 dex, and the difference between this work and CM05 is also found to be lower (by -0.17 dex). There is only one common Zn line between this work and CM05; this line differs in both EW (by 17$\%$) and in log(gf) value (by 0.05 dex).

The M13 star also shows most 