We present the results of an X-ray spectral analysis of 153 galaxy clusters observed with the Chandra, XMM-Newton, and Suzaku space telescopes. These clusters, which span 0 500) ICM metallicity (dZ/dz = -0.06 ± 0.04 Z ?), with a mean value at z = 0.6 of =0.23+/- 0.01 Z ? and a scatter of s Z = 0.08 ± 0.01 Z ?. These results imply that the emission-weighted metallicity has not changed by more than 40%25 since z = 1 (at 95%25 confidence), consistent with the picture of an early (z %26gt; 1) enrichment. We find, in agreement with previous works, a significantly higher mean value for the metallicity in the centers of cool core clusters versus non-cool core clusters. We find weak evidence for evolution in the central metallicity of cool core clusters (dZ/dz = -0.21 ± 0.11 Z ?), which is sufficient to account for this enhanced central metallicity over the past ˜10 Gyr. We find no evidence for metallicity evolution outside of the core (dZ/dz = -0.03 ± 0.06 Z ?), and no significant difference in the core-excised metallicity between cool core and non-cool core clusters. This suggests that strong radio-mode active galactic nucleus feedback does not significantly alter the distribution of metals at r\gt 0.15{R}500. Given the limitations of current-generation X-ray telescopes in constraining the ICM metallicity at z %26gt; 1, significant improvements on this work will likely require next-generation X-ray missions.
We present the results of an X-ray spectral analysis of 153 galaxy clusters observed with the Chandra, XMM-Newton, and Suzaku space telescopes. These clusters, which span 0 500) ICM metallicity (dZ/dz = -0.06 ± 0.04 Z ⊙), with a mean value at z = 0.6 of =0.23 /- 0.01 Z ⊙ and a scatter of σ Z = 0.08 ± 0.01 Z ⊙. These results imply that the emission-weighted metallicity has not changed by more than 40% since z = 1 (at 95% confidence), consistent with the picture of an early (z > 1) enrichment. We find, in agreement with previous works, a significantly higher mean value for the metallicity in the centers of cool core clusters versus non-cool core clusters. We find weak evidence for evolution in the central metallicity of cool core clusters (dZ/dz = -0.21 ± 0.11 Z ⊙), which is sufficient to account for this enhanced central metallicity over the past ˜10 Gyr. We find no evidence for metallicity evolution outside of the core (dZ/dz = -0.03 ± 0.06 Z ⊙), and no significant difference in the core-excised metallicity between cool core and non-cool core clusters. This suggests that strong radio-mode active galactic nucleus feedback does not significantly alter the distribution of metals at r\gt 0.15{R}500. Given the limitations of current-generation X-ray telescopes in constraining the ICM metallicity at z > 1, significant improvements on this work will likely require next-generation X-ray missions.
