We compare our compilation of the W ′ calcium index for 71 Galactic globular clusters to the widely used Zinn and West (1984 ApJS, 55, 45) [Fe/H] scale and to Carretta and Gratton's (1997 A&AS, 121, 95) scale from high-dispersion spectra analyzed with Kurucz (1992, private communication) model atmospheres. We find our calcium ranking to be tightly correlated with each comparison set, in a non-linear and a linear fashion, respectively. By combining our calcium index information with the Zinn and West ranking, we are able to rank the globular clusters in our sample with a typical precision of ±0.05 dex for [Fe/H] ZW 84 ∼ < −0.5; for clusters more metal rich than this, the ranking is less precise. The significant differences between these metallicity scales raise important questions about our understanding of Galactic formation and chemical enrichment processes. Furthermore, in spite of the apparent improvement in metallicity ranking for the Galactic globular clusters that results from our addition of information from the Ca II triplet lines to the potpourri of other metallicity indicators, caution -perhaps considerable -may be advisable when using W ′ as a surrogate for metallicity, especially for systems where ranges in age and metallicity are likely.

The average mass density profile measured in the CNOC cluster survey is well described with the analytic form ρ(r) = Ar −1 (r + a ρ ) −2 , as advocated on the basis on n-body simulations by Navarro, Frenk & White. The predicted core radii are a ρ = 0.20 (in units of the radius where the mean interior density is 200 times the critical density) for an Ω = 0.2 open CDM model, or a ρ = 0.26 for a flat Ω = 0.2 model, with little dependence on other cosmological parameters for simulations normalized to the observed cluster abundance. The dynamically derived local mass-to-light ratio, which has little radial variation, converts the observed light profile to a mass profile. We find that the scale radius of the mass distribution, 0.20 ≤ a ρ ≤ 0.30 (depending on modeling details, with a 95% confidence range of 0.12 − 0.50), is completely consistent with the predicted values. Moreover, the profiles and total masses of the clusters as individuals can be acceptably predicted from the cluster RMS line-of-sight velocity dispersion alone. This is strong support of the hierarchical clustering theory for the formation of galaxy clusters in a cool, collisionless, dark matter dominated universe.Subject headings: galaxies: clusters, cosmology: large-scale structure of universe 1 Visiting Astronomer, Canada-France-Hawaii Telescope, which is operated by the National

ABSTRACT. We present accurate photometry on the Johnson B, Kron-Cousins R photometric system for approximately 100,000 stars in a deg 2 field centered on the dwarf spheroidal galaxy in Fornax. We identify 1 3 numerous probable short-period variable stars, blue stars that appear to be the main sequence of a small population with an age of order 10 8 yr, and two distinct types of luminous red star: an extended sequence of primarily carbon stars and a clump of mostly M giants slightly more luminous than the giant-branch tip. The spatial distribution of each of these subpopulations within the Fornax dwarf galaxy is considered.