covers a wide range in color, this extended sequence was not visible in either previous work and represents a significant change in the picture of the M32 RGB. The present CM diagram is consistent, however, with Freedman’s noted incompleteness at faint [*V*]{} magnitudes and her corresponding insensitivity to very red stars. This insensitivity is obvious when one considers the effect of a [*V*]{}-magnitude limit given the morphology apparent in the [*V*]{} vs diagram, illustrated in Figure \[fig:cmtracks\]. In short, the new [*HST*]{} measurements reveal the full extent and morphology of the upper giant branch for the first time. Even with [*HST,*]{} however, there may be some incompleteness for very red stars with $ > 3$. For example, we find 14 starlike objects brighter than $I=22$ that have no visible counterparts at all in the F555W image. Most of these are probably extremely red giants with $>4$).

Below about $I = 22,$ the giant stars appear to merge into a rather fat giant branch of more or less uniform width down almost to the clump. Based on the completeness tests, the width of the giant branch above [*I*]{} $\sim 24$ is significantly larger than can be accounted for by photometric errors 