The history of metal enrichment traced by X-ray observations of high-redshift galaxy clusters

Flores, Anthony M.; Mantz, Adam B.; Allen, Steven W.; Morris, R. Glenn; Canning, Rebecca E. A.; Bleem, Lindsey E.; Calzadilla, Michael S.; Floyd, Benjamin T.; McDonald, Michael; Ruppin, Florian

doi:10.1093/mnras/stab2430

The history of metal enrichment traced by X-ray observations of high-redshift galaxy clusters

Journal Article · Mon Aug 30 00:00:00 EDT 2021 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stab2430· OSTI ID:1820197

; ; Allen, Steven W.; Morris, R. Glenn; Canning, Rebecca E. A.; Bleem, Lindsey E.; Calzadilla, Michael S.; ; McDonald, Michael;

ABSTRACT

We present the analysis of deep X-ray observations of 10 massive galaxy clusters at redshifts 1.05 < z < 1.71, with the primary goal of measuring the metallicity of the intracluster medium (ICM) at intermediate radii, to better constrain models of the metal enrichment of the intergalactic medium. The targets were selected from X-ray and Sunyaev–Zel’dovich effect surveys, and observed with both the XMM–Newton and Chandra satellites. For each cluster, a precise gas mass profile was extracted, from which the value of r500 could be estimated. This allows us to define consistent radial ranges over which the metallicity measurements can be compared. In general, the data are of sufficient quality to extract meaningful metallicity measurements in two radial bins, r < 0.3r500 and 0.3 < r/r500 < 1.0. For the outer bin, the combined measurement for all 10 clusters, Z/Z⊙ = 0.21 ± 0.09, represents a substantial improvement in precision over previous results. This measurement is consistent with, but slightly lower than, the average metallicity of 0.315 solar measured at intermediate-to-large radii in low-redshift clusters. Combining our new high-redshift data with the previous low-redshift results allows us to place the tightest constraints to date on models of the evolution of cluster metallicity at intermediate radii. Adopting a power-law model of the form Z ∝ (1 + z)γ, we measure a slope $$\gamma = -0.5^{+0.4}_{-0.3}$$, consistent with the majority of the enrichment of the ICM having occurred at very early times and before massive clusters formed, but leaving open the possibility that some additional enrichment in these regions may have occurred since a redshift of 2.

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Research Organization:: Argonne National Laboratory (ANL), Argonne, IL (United States); SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)

Sponsoring Organization:: Gordon and Betty Moore Foundation; National Aeronautics and Space Administration (NASA); National Science Foundation (NSF); Swiss National Science Foundation (SNSF); USDOE; USDOE Office of Science (SC)

Grant/Contract Number:: AC02-06CH11357; AC02-76SF00515

OSTI ID:: 1820197

Alternate ID(s):: OSTI ID: 1923055

Journal Information:: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 4 Vol. 507; ISSN 0035-8711

Publisher:: Oxford University PressCopyright Statement

Country of Publication:: United Kingdom

Language:: English

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