The Remarkable Similarity of Massive Galaxy Clusters From z~0 to z~1.9
We present the results of a Chandra X-ray survey of the 8 most massive galaxy clusters at z>1.2 in the South Pole Telescope 2500 deg^2 survey. We combine this sample with previously-published Chandra observations of 49 massive X-ray-selected clusters at 00.2R500 scaling like E(z)^2. In the center...
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ftdatacite:10.48550/arxiv.1702.05094 2023-05-15T18:22:54+02:00 The Remarkable Similarity of Massive Galaxy Clusters From z~0 to z~1.9 McDonald, 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. 2017 https://dx.doi.org/10.48550/arxiv.1702.05094 https://arxiv.org/abs/1702.05094 unknown arXiv https://dx.doi.org/10.3847/1538-4357/aa7740 arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences article-journal Article ScholarlyArticle Text 2017 ftdatacite https://doi.org/10.48550/arxiv.1702.05094 https://doi.org/10.3847/1538-4357/aa7740 2022-04-01T10:41:18Z We present the results of a Chandra X-ray survey of the 8 most massive galaxy clusters at z>1.2 in the South Pole Telescope 2500 deg^2 survey. We combine this sample with previously-published Chandra observations of 49 massive X-ray-selected clusters at 00.2R500 scaling like E(z)^2. In the centers of clusters (r<0.1R500), we find significant deviations from self similarity (n_e ~ E(z)^{0.1+/-0.5}), consistent with no redshift dependence. When we isolate clusters with over-dense cores (i.e., cool cores), we find that the average over-density 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)^(-1). : 14 pages, 12 figures, 3 tables. Submitted to ApJ. Comments welcome Text South pole DataCite Metadata Store (German National Library of Science and Technology) South Pole |
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DataCite Metadata Store (German National Library of Science and Technology) |
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Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences |
spellingShingle |
Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences McDonald, 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. The Remarkable Similarity of Massive Galaxy Clusters From z~0 to z~1.9 |
topic_facet |
Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences |
description |
We present the results of a Chandra X-ray survey of the 8 most massive galaxy clusters at z>1.2 in the South Pole Telescope 2500 deg^2 survey. We combine this sample with previously-published Chandra observations of 49 massive X-ray-selected clusters at 00.2R500 scaling like E(z)^2. In the centers of clusters (r<0.1R500), we find significant deviations from self similarity (n_e ~ E(z)^{0.1+/-0.5}), consistent with no redshift dependence. When we isolate clusters with over-dense cores (i.e., cool cores), we find that the average over-density 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)^(-1). : 14 pages, 12 figures, 3 tables. Submitted to ApJ. Comments welcome |
format |
Text |
author |
McDonald, 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. |
author_facet |
McDonald, 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. |
author_sort |
McDonald, M. |
title |
The Remarkable Similarity of Massive Galaxy Clusters From z~0 to z~1.9 |
title_short |
The Remarkable Similarity of Massive Galaxy Clusters From z~0 to z~1.9 |
title_full |
The Remarkable Similarity of Massive Galaxy Clusters From z~0 to z~1.9 |
title_fullStr |
The Remarkable Similarity of Massive Galaxy Clusters From z~0 to z~1.9 |
title_full_unstemmed |
The Remarkable Similarity of Massive Galaxy Clusters From z~0 to z~1.9 |
title_sort |
remarkable similarity of massive galaxy clusters from z~0 to z~1.9 |
publisher |
arXiv |
publishDate |
2017 |
url |
https://dx.doi.org/10.48550/arxiv.1702.05094 https://arxiv.org/abs/1702.05094 |
geographic |
South Pole |
geographic_facet |
South Pole |
genre |
South pole |
genre_facet |
South pole |
op_relation |
https://dx.doi.org/10.3847/1538-4357/aa7740 |
op_rights |
arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ |
op_doi |
https://doi.org/10.48550/arxiv.1702.05094 https://doi.org/10.3847/1538-4357/aa7740 |
_version_ |
1766202308155146240 |