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We present the analysis of deep X-ray observations of 10 massive galaxyclusters at redshifts $1.05 < z < 1.71$, with the primary goal of measuring themetallicity of the intracluster medium (ICM) at intermediate radii, to betterconstrain models of the metal enrichment of the intergalactic medium. Thetargets were selected from X-ray and Sunyaev-Zel'dovich (SZ) effect surveys,and observed with both the \textit{XMM-Newton} and \textit{Chandra} satellites.For each cluster, a precise gas mass profile was extracted, from which thevalue of $r_{500}$ could be estimated. This allows us to define consistentradial ranges over which the metallicity measurements can be compared. Ingeneral, the data are of sufficient quality to extract meaningful metallicitymeasurements in two radial bins, $r<0.3r_{500}$ and $0.3<r/r_{500}<1.0$. Forthe outer bin, the combined measurement for all ten clusters, $Z/Z_{\odot} =0.21 \pm 0.09$, represents a substantial improvement in precision over previousresults. This measurement is consistent with, but slightly lower than, theaverage metallicity of 0.315 Solar measured at intermediate-to-large radii inlow-redshift clusters. Combining our new high-redshift data with the previouslow-redshift results allows us to place the tightest constraints to date onmodels of the evolution of cluster metallicity at intermediate radii. Adoptinga power law model of the form $Z \propto \left(1+z\right)^\gamma$, we measure aslope $\gamma = -0.5^{+0.4}_{-0.3}$, consistent with the majority of theenrichment of the ICM having occurred at very early times and before massiveclusters formed, but leaving open the possibility that some additionalenrichment in these regions may have occurred since a redshift of 2.

The History of Metal Enrichment Traced by X-ray Observations of High Redshift Galaxy Clusters