First is the CO index as computed by Doyon et al. Next are two computations of the CaII IR triplet using the relations of Diaz et al. Next come the 1.62 and 2.29 micron CO features, and the 1.59 micron Si feature, which were modeled for individual stars by Origlia et al. This subroutine is still under construction. Eventually it will compute the stellar absorption spectrum of the higher Balmer lines.
Quantities given are the line fluxes and the equivalent widths.
When in doubt, compute all the output files. This will work.