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We study the evolution of the ICM with a sample of 70 galaxy clustersspanning 0.18 < z < 1.24. We find that X-ray luminosity and ICM mass at a fixedtemperature evolve with redshift in a manner inconsistent with the standardself-similar model of cluster formation. Both luminosity and ICM mass evolvemore slowly toward high redshift than the self-similar prediction. We find thatevolution in these two observables can be modeled by a simple evolution in thecluster gas mass fraction. Excluding cluster cores from measurements results inevolution more consistent with the self-similar model than when the entirecluster is used, indicating that the fraction of clusters with cool coresincreases with time, or that cool cores become more developed over time inthose clusters that have them; this is supported by direct study of theredshift dependence of central surface brightness, which increases in scatterand magnitude at low redshift. We find that isophotal size-temperaturerelations evolve differently according to which isophote is used, indicatingthat the central and outer regions of cluster ICM evolve differently. We showthat constraints on the evolution of the gas fraction and isophotalsize-temperature relations constraints can be combined to measure clusterdistances, and thus to constrain cosmological parameters. There are indicationsthat scaling relation scatter decreases at higher redshift, suggesting thatmerging is not the dominant source of cluster structural variation. Our resultsprovide constraints for simulations attempting to model cluster physics,indicate some difficulties for cosmological studies that assume constantcluster gas fractions, and point toward other potentially more robust uses ofclusters for cosmological applications. (Abridged)

Evolution of the Intracluster Medium Between 0.2 < z < 1.3 in a Chandra Sample of 70 Galaxy Clusters