Phase diagrams for runs CSFSN (left) and CSFSNBF (right) at 30 Myr. The color coding shows particle numbers, so that brighter regions have more particles in the corresponding range of density and temperature. The overall morphology is similar between the two runs, but a larger fraction of the gas clearly can reach higher temperatures in the AGN feedback case, as shown by the fact that the diagram is more densely populated above ﹩{10}^{5.5}﹩ K. Other differences are likely related to the intrinsic stochasticity of star formation and SN feedback.