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dc.contributor.authorAllen, S. W.
dc.contributor.authorBenson, B. A.
dc.contributor.authorBleem, L. E.
dc.contributor.authorBrodwin, M.
dc.contributor.authorCarlstrom, J. E.
dc.contributor.authorForman, W. R.
dc.contributor.authorHlavacek-Larrondo, J.
dc.contributor.authorGarmire, G. P.
dc.contributor.authorGaspari, M.
dc.contributor.authorGladders, M. D.
dc.contributor.authorMantz, A. B.
dc.contributor.authorMurray, S. S.
dc.contributor.authorMcDonald, Michael A.
dc.contributor.authorBayliss, Matthew B
dc.contributor.authorBulbul, Gul E
dc.date.accessioned2018-02-26T16:18:37Z
dc.date.available2018-02-26T16:18:37Z
dc.date.issued2017-06
dc.identifier.issn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1721.1/113884
dc.description.abstractWe present the results of a Chandra X-ray survey of the eight most massive galaxy clusters at z > 1.2 in the South Pole Telescope 2500 deg[superscript 2] survey. We combine this sample with previously published Chandra observations of 49 massive X-ray-selected clusters at 0 < z < 0.1 and 90 Sunyaev-Zel'dovich-selected clusters at 0.25 < z < 1.2 to constrain the evolution of the intracluster medium (ICM) over the past ∼10 Gyr. We find that the bulk of the ICM has evolved self-similarly over the full redshift range probed here, with the ICM density at r > 0.2R[subscript 500] scaling like E(Z)[superscript 2]. In the centers of clusters (r ≲ 0.01R[subscript 500]), we find significant deviations from self-similarity (n[subscript e] ∝ E(z)[superscript 0.2±0.5]), consistent with no redshift dependence. When we isolate clusters with overdense cores (i.e., cool cores), we find that the average overdensity profile has not evolved with redshift - that is, cool cores have not changed in size, density, or total mass over the past ∼9-10 Gyr. We show that the evolving "cuspiness" of clusters in the X-ray, reported by several previous studies, can be understood in the context of a cool core with fixed properties embedded in a self-similarly evolving cluster. We find no measurable evolution in the X-ray morphology of massive clusters, seemingly in tension with the rapidly rising (with redshift) rate of major mergers predicted by cosmological simulations. We show that these two results can be brought into agreement if we assume that the relaxation time after a merger is proportional to the crossing time, since the latter is proportional to H(Z)[superscript -1] .en_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.isversionofhttp://dx.doi.org/10.3847/1538-4357/AA7740en_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.titleThe Remarkable Similarity of Massive Galaxy Clusters from z ~ 0 to z ~ 1.9en_US
dc.typeArticleen_US
dc.identifier.citationMcDonald, M., et al. “The Remarkable Similarity of Massive Galaxy Clusters from z ∼ 0 to z ∼ 1.9.” The Astrophysical Journal, vol. 843, no. 1, June 2017, p. 28. © 2017 The American Astronomical Societyen_US
dc.contributor.departmentMassachusetts Institute of Technology. Department of Physicsen_US
dc.contributor.departmentMIT Kavli Institute for Astrophysics and Space Researchen_US
dc.contributor.mitauthorMcDonald, Michael A.
dc.contributor.mitauthorBayliss, Matthew B
dc.contributor.mitauthorBulbul, Gul E
dc.relation.journalThe Astrophysical Journalen_US
dc.eprint.versionFinal published versionen_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dc.date.updated2018-02-16T14:50:41Z
dspace.orderedauthorsMcDonald, M.; Allen, S. W.; Bayliss, M.; Benson, B. A.; Bleem, L. E.; Brodwin, M.; Bulbul, E.; Carlstrom, J. E.; Forman, W. R.; Hlavacek-Larrondo, J.; Garmire, G. P.; Gaspari, M.; Gladders, M. D.; Mantz, A. B.; Murray, S. S.en_US
dspace.embargo.termsNen_US
dc.identifier.orcidhttps://orcid.org/0000-0001-5226-8349
mit.licensePUBLISHER_POLICYen_US


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