Based on observations collected at the European Southern Observatory, Chile, 67.D-0086A, and the German Spanish Astronomical Center, Calar Alto, Spain.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

Of the three IR triplet lines, we look only at Ca II $\lambda~8498$ , as a) it is the weakest of the three and b) it is least perturbed by Paschen lines.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... $_{\rm II}$

The subscript in [X/Y] $_{\rm II}$ indicates that the abundance for element X is determined from the singly ionized species. Likewise, a subscript I refers to neutral lines used in the abundance determination.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.