An accurate, easy-to-use abundance scale for globular clusters based on 2.2 micron spectra of giant stars

We present a new method for the determination of [Fe/H] for globular cluste rs. This method is based on moderate-resolution (similar to 1500) near-IR s pectroscopy in the K band of six to 10 of the brightest giants in a cluster . Our final [Fe/H] calibration is derived from spectra of 105 stars in 15 g lobular clusters with [Fe/H] ranging from near solar to -1.8. We measure th e equivalent widths of three features in these spectra, EW(Na), EW(Ca), and EW(CO). Our calibration reproduces the Zinn & West abundance scale as upda ted by Harris to better than +/-0.10 dex. A quadratic Dt to the data is som ewhat better than a simple linear fit. Three advantages of this new method are that it can be used for metal-rich, heavily reddened globular clusters in crowded fields; it does not require any knowledge of any other cluster o r stellar parameter, such as reddening, distance, or luminosity; and it doe s not require much telescope time. If stellar (J-K)(0) and M-K values are available in addition to the near-IR spectra, the accuracy of the [Fe/H] value derived is further improved. If observations-either near-IR spectra alone or spectra plus colors and magnit udes-of only three stars in a cluster are available, the resulting value of [Fe/H] will be nearly as reliable as the application of our new technique to 2 to 3 times as many stars. The accuracy of an [Fe/H] value based on obs ervations of CO absorption by itself is significantly less than that which results from the three spectroscopic indices, in spite of the fact that the CO feature is by far the strongest feature in the spectrum. There are two probable reasons for this. First, the CO bands approach saturation for brig ht giants in high-metallicity clusters. Second, within a cluster there is c onsiderable intrinsic star-to-star scatter in EW(CO) due to differences in mixing histories on the giant branch. In contrast, we do not find evidence for any intrinsic scatter in the Na or Ca indices. Nevertheless, we predict that observations from space of CO absorption in the integrated light of s tellar systems will prove to be of great value for abundance determinations at least as distant as the Coma cluster of galaxies. Finally, a comparison of globular cluster abundances based on high-resolution spectroscopy with the Zinn & West/Harris [Fe/H] scale-and by inference ours-leads us to concl ude that the two are closely linearly related over the entire range of glob ular cluster abundances, although there might be a small, constant offset b etween the two.