The Evolution of Structure in X-ray Clusters of Galaxies
Using Chandra archival data, we quantify the evolution of cluster morphology with redshift. Clusters form and grow through mergers with other clusters and groups, and the amount of substructure in clusters in the present epoch and how quickly it evolves with redshift depend on the underlying cosmolo...
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| Format: | Article |
| Language: | en_US |
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IOP Publishing
2012
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| Online Access: | http://hdl.handle.net/1721.1/71917 https://orcid.org/0000-0002-1379-4482 https://orcid.org/0000-0002-5769-8441 |
| _version_ | 1826212605006446592 |
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| author | Jeltema, Tesla E. Canizares, Claude R. Buote, David A. Bautz, Marshall W. |
| author2 | MIT Kavli Institute for Astrophysics and Space Research |
| author_facet | MIT Kavli Institute for Astrophysics and Space Research Jeltema, Tesla E. Canizares, Claude R. Buote, David A. Bautz, Marshall W. |
| author_sort | Jeltema, Tesla E. |
| collection | MIT |
| description | Using Chandra archival data, we quantify the evolution of cluster morphology with redshift. Clusters form and grow through mergers with other clusters and groups, and the amount of substructure in clusters in the present epoch and how quickly it evolves with redshift depend on the underlying cosmology. Our sample includes 40 X-ray-selected, luminous clusters from the Chandra archive, and we quantify cluster morphology using the power ratio method of Buote & Tsai. The power ratios are constructed from the moments of the X-ray surface brightness and are related to a cluster's dynamical state. We find that, as expected qualitatively from hierarchical models of structure formation, high-redshift clusters have more substructure and are dynamically more active than low-redshift clusters. Specifically, the clusters with z > 0.5 have significantly higher average third- and fourth-order power ratios than the lower redshift clusters. Of the power ratios, P[subscript 3]/P[subscript 0] is the most unambiguous indicator of an asymmetric cluster structure, and the difference in P[subscript 3]/P[subscript 0] between the two samples remains significant even when the effects of noise and other systematics are considered. After correcting for noise, we apply a linear fit to P[subscript 3]/P[subscript 0] versus redshift and find that the slope is greater than zero at better than 99% confidence. This observation of structure evolution indicates that dynamical state may be an important systematic effect in cluster studies seeking to constrain cosmology, and when calibrated against numerical simulations, structure evolution will itself provide interesting bounds on cosmological models. |
| first_indexed | 2024-09-23T15:29:21Z |
| format | Article |
| id | mit-1721.1/71917 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T15:29:21Z |
| publishDate | 2012 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/719172022-09-29T14:45:55Z The Evolution of Structure in X-ray Clusters of Galaxies Jeltema, Tesla E. Canizares, Claude R. Buote, David A. Bautz, Marshall W. MIT Kavli Institute for Astrophysics and Space Research Canizares, Claude R. Jeltema, Tesla E. Canizares, Claude R. Bautz, Mark W. Using Chandra archival data, we quantify the evolution of cluster morphology with redshift. Clusters form and grow through mergers with other clusters and groups, and the amount of substructure in clusters in the present epoch and how quickly it evolves with redshift depend on the underlying cosmology. Our sample includes 40 X-ray-selected, luminous clusters from the Chandra archive, and we quantify cluster morphology using the power ratio method of Buote & Tsai. The power ratios are constructed from the moments of the X-ray surface brightness and are related to a cluster's dynamical state. We find that, as expected qualitatively from hierarchical models of structure formation, high-redshift clusters have more substructure and are dynamically more active than low-redshift clusters. Specifically, the clusters with z > 0.5 have significantly higher average third- and fourth-order power ratios than the lower redshift clusters. Of the power ratios, P[subscript 3]/P[subscript 0] is the most unambiguous indicator of an asymmetric cluster structure, and the difference in P[subscript 3]/P[subscript 0] between the two samples remains significant even when the effects of noise and other systematics are considered. After correcting for noise, we apply a linear fit to P[subscript 3]/P[subscript 0] versus redshift and find that the slope is greater than zero at better than 99% confidence. This observation of structure evolution indicates that dynamical state may be an important systematic effect in cluster studies seeking to constrain cosmology, and when calibrated against numerical simulations, structure evolution will itself provide interesting bounds on cosmological models. United States. National Aeronautics and Space Administration. (Contract Number NAS8-01129) 2012-07-31T17:34:37Z 2012-07-31T17:34:37Z 2005-05 2004-11 Article http://purl.org/eprint/type/JournalArticle 0004-637X 1538-4357 http://hdl.handle.net/1721.1/71917 Jeltema, Tesla E. et al. “The Evolution of Structure in X‐Ray Clusters of Galaxies.” The Astrophysical Journal 624.2 (2005): 606–629. https://orcid.org/0000-0002-1379-4482 https://orcid.org/0000-0002-5769-8441 en_US http://dx.doi.org/10.1086/428940 Astrophysical Journal Article 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. application/pdf IOP Publishing arVix |
| spellingShingle | Jeltema, Tesla E. Canizares, Claude R. Buote, David A. Bautz, Marshall W. The Evolution of Structure in X-ray Clusters of Galaxies |
| title | The Evolution of Structure in X-ray Clusters of Galaxies |
| title_full | The Evolution of Structure in X-ray Clusters of Galaxies |
| title_fullStr | The Evolution of Structure in X-ray Clusters of Galaxies |
| title_full_unstemmed | The Evolution of Structure in X-ray Clusters of Galaxies |
| title_short | The Evolution of Structure in X-ray Clusters of Galaxies |
| title_sort | evolution of structure in x ray clusters of galaxies |
| url | http://hdl.handle.net/1721.1/71917 https://orcid.org/0000-0002-1379-4482 https://orcid.org/0000-0002-5769-8441 |
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