Deep XMM–Newton observations of the most distant SPT-SZ galaxy cluster

Journal Article · 05 June 2020 · Monthly Notices of the Royal Astronomical Society

DOI: https://doi.org/10.1093/mnras/staa1581 · OSTI ID:1635044

Mantz, Adam B.  ^[1]; Allen, Steven W. ^[2]; Morris, R. Glenn ^[2]; Canning, Rebecca E. A. ^[1]; Bayliss, Matthew ^[3]; Bleem, Lindsey E. ^[4]; Floyd, Benjamin T.  ^[5]; McDonald, Michael ^[6]

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1. Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, CA 94305, USA, Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA
2. Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, CA 94305, USA, Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025, USA
3. Department of Physics, University of Cincinnati, Cincinnati, OH 45221, USA
4. HEP Division, Argonne National Laboratory, Argonne, IL 60439, USA, Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA
5. Department of Physics and Astronomy, University of Missouri, 5110 Rockhill Road, Kansas City, MO 64110, USA
6. Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA

ABSTRACT We present results from a 577 ks XMM–Newton observation of SPT-CL J0459–4947, the most distant cluster detected in the South Pole Telescope 2500 square degree (SPT-SZ) survey, and currently the most distant cluster discovered through its Sunyaev–Zel’dovich effect. The data confirm the cluster’s high redshift, z = 1.71 ± 0.02, in agreement with earlier, less precise optical/IR photometric estimates. From the gas density profile, we estimate a characteristic mass of $$M_{500}=(1.8\pm 0.2)\times 10^{14}\, {\rm M}_{\odot }$$; cluster emission is detected above the background to a radius of $$\sim \!2.2\, r_{500}$$, or approximately the virial radius. The intracluster gas is characterized by an emission-weighted average temperature of 7.2 ± 0.3 keV and metallicity with respect to Solar of $$Z/\, Z_{\odot }=0.37\pm 0.08$$. For the first time at such high redshift, this deep data set provides a measurement of metallicity outside the cluster centre; at radii $$r\gt 0.3\, r_{500}$$, we find $$Z/\, Z_{\odot }=0.33\pm 0.17$$ in good agreement with precise measurements at similar radii in the most nearby clusters, supporting an early enrichment scenario in which the bulk of the cluster gas is enriched to a universal metallicity prior to cluster formation, with little to no evolution thereafter. The leverage provided by the high redshift of this cluster tightens by a factor of 2 constraints on evolving metallicity models, when combined with previous measurements at lower redshifts.

• Research Organization: Argonne National Laboratory (ANL), Argonne, IL (United States)
• Sponsoring Organization: National Aeronautic and Space Administration (NASA); National Science Foundation (NSF); USDOE; USDOE Office of Science (SC), Basic Energy Sciences (BES)
• Grant/Contract Number: AC02-06CH11357; AC02-76SF00515
• OSTI ID: 1635044
• Journal Information: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 2 Vol. 496; ISSN 0035-8711
• Publisher: Royal Astronomical SocietyCopyright Statement
• Country of Publication: United Kingdom
• Language: English