(the color uncertainty at $I = 23$ is 0.125 mag RMS, whereas the observed giant branch width at this point is 0.253 mag RMS — we return to this point below). The core-helium burning stars seem to be concentrated in a red clump. We see no indications of RR Lyraes or an extended reddish horizontal branch, even though the completeness in the region of the diagram where they should appear ([*I*]{} $\sim 24.6$, $\sim 0.5$) is $\sim$65%. The form of the fall-off in the density of stars below $I = 25$ is due to a combination of completeness effects and photometric uncertainties.

Crowding and the Brightest Giants \[sec:crowding\]
--------------------------------------------------

We observe a significant number of stars to be brighter than the first ascent RGB tip. These may be AGB stars. However, their luminosities are significantly fainter than the AGB stars identified by Freedman (1989). Assuming a distance modulus $(m-M)_0 = 24.43$ (Ajhar 1996), we expect the tip of the giant branch for older/more metal-poor populations to occur at $I\approx 20.4$. We find 23 stars with $I <
20.4$ in POS1 and only one such star in POS2, giving a surface density of AGB stars of 70 arcmin$^{-2}$. Though the absence 