elements agree within the errors with the exception of Na, and V (which lie within 2 $\sigma$), of Ti, Ni, and Y (3 $\sigma$), and of Al, and Ca (4 $\sigma$). The Na abundances are computed from log(gf) values that differ with CM05 by up to 0.05 dex and with excitation potentials that differ by up to 0.10 ev. V, Ni, Ca, and La derived abundances share the same discrepancies discussed above with the M3 standard star. The Ti abundance is calculated from an average between TiI and TiII and in this work there are many more TiII lines than with CM05. The NLTE effects on TiI are well known and result in a lower TiI abundance compared to TiII (see Section \[sec:tidiff\]), thus an average computed with more TiI lines than TiII (such as CM05) will inevitably ensure an overall lower Ti abundance as is shown for both standard stars. The Y abundance is derived from 4 lines, 3 of which are in common with CM05; the line that is not in common with CM05 yields a higher abundance by $\sim$ 0.2 dex. The Al abundance is derived from entirely different lines than CM05. For La there are only 