is fairly smooth, but with many more metal-rich stars than metal-poor ones. This is illustrated in Figure \[fig:hist\], where we compute the metallicity histogram by laying down a mesh of 10 Gyr isochrones on the CM diagram covering a wide range of \[Fe/H\], and then counting the stars between them brighter than $M_I=-2.4$, where the uncertainties are fairly small. A small correction for differences in RGB lifetime at different metallicities was also applied. No correction was applied for [*V*]{}-band incompleteness for the reddest giants, so the highest metallicity bins slightly underestimate the true number of giants by up to 14 stars. One sees that the majority of stars lie along the red side of the RGB, with a decreasing tail toward blue, metal-poor RGB loci. There are very few stars ($<1$%) more metal-poor than \[Fe/H\]$\approx -1.5$. Although some of us initially had a visual impression of bimodality in the CM diagram, with a slight paucity of stars between the main “blue” and “red” RGBs, the \[Fe/H\] distribution shows no evidence of this. The illusion probably stems from the fact that RGB color begins to change rapidly with metallicity at about \[Fe/H\]$ =-0.5$ and higher. The effect of assuming a population 