Projected two-temperature fits showing the presence of a cooler component toward the center of four of our clusters. Shown in red is the radial extent of the Hα nebular emission reported by McDonald et al. (2010). A2029 showed no requirement for a second temperature component, hence its omission here. Note that these temperature measurements are likely overestimated—the resulting counts after deprojection meant that two-temperature models could only be successfully fitted for the projected spectra. Nevertheless, cooling gas is recovered in all systems with known Hα. Furthermore there is tentative evidence for a relation between the extent of Hα and that of the cooler X-ray component.