Impact of Cluster Physics on the Sunyaev-Zel'dovich Power Spectrum
We use an analytic model to investigate the theoretical uncertainty on the thermal Sunyaev-Zel'dovich (SZ) power spectrum due to astrophysical uncertainties in the thermal structure of the intracluster medium. Our model accounts for star formation and energy feedback (from supernovae and active...
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ftdatacite:10.48550/arxiv.1006.1945 2023-05-15T18:23:08+02:00 Impact of Cluster Physics on the Sunyaev-Zel'dovich Power Spectrum Shaw, Laurie D. Nagai, Daisuke Bhattacharya, Suman Lau, Erwin T. 2010 https://dx.doi.org/10.48550/arxiv.1006.1945 https://arxiv.org/abs/1006.1945 unknown arXiv https://dx.doi.org/10.1088/0004-637x/725/2/1452 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 2010 ftdatacite https://doi.org/10.48550/arxiv.1006.1945 https://doi.org/10.1088/0004-637x/725/2/1452 2022-04-01T14:22:41Z We use an analytic model to investigate the theoretical uncertainty on the thermal Sunyaev-Zel'dovich (SZ) power spectrum due to astrophysical uncertainties in the thermal structure of the intracluster medium. Our model accounts for star formation and energy feedback (from supernovae and active galactic nuclei) as well as radially dependent non-thermal pressure support due to random gas motions, the latter calibrated by recent hydrodynamical simulations. We compare the model against X-ray observations of low redshift clusters, finding excellent agreement with observed pressure profiles. Varying the levels of feedback and non-thermal pressure support can significantly change both the amplitude and shape of the thermal SZ power spectrum. Increasing the feedback suppresses power at small angular scales, shifting the peak of the power spectrum to lower ell. On the other hand, increasing the non-thermal pressure support has the opposite effect, significantly reducing power at large angular scales. In general, including non-thermal pressure at the level measured in simulations has a large effect on the power spectrum, reducing the amplitude by 50% at angular scales of a few arcminutes compared to a model without a non-thermal component. Our results demonstrate that measurements of the shape of the power spectrum can reveal useful information on important physical processes in groups and clusters, especially at high-redshift where there exists little observational data. Comparing with the recent South Pole Telescope measurements of the small-scale cosmic microwave background power spectrum, we find our model reduces the tension between the values of sigma_8 measured from the SZ power spectrum and from cluster abundances. : 15 Pages, 9 Figures, updated to match version accepted by ApJ Text South pole DataCite Metadata Store (German National Library of Science and Technology) South Pole |
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Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences |
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Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences Shaw, Laurie D. Nagai, Daisuke Bhattacharya, Suman Lau, Erwin T. Impact of Cluster Physics on the Sunyaev-Zel'dovich Power Spectrum |
topic_facet |
Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences |
description |
We use an analytic model to investigate the theoretical uncertainty on the thermal Sunyaev-Zel'dovich (SZ) power spectrum due to astrophysical uncertainties in the thermal structure of the intracluster medium. Our model accounts for star formation and energy feedback (from supernovae and active galactic nuclei) as well as radially dependent non-thermal pressure support due to random gas motions, the latter calibrated by recent hydrodynamical simulations. We compare the model against X-ray observations of low redshift clusters, finding excellent agreement with observed pressure profiles. Varying the levels of feedback and non-thermal pressure support can significantly change both the amplitude and shape of the thermal SZ power spectrum. Increasing the feedback suppresses power at small angular scales, shifting the peak of the power spectrum to lower ell. On the other hand, increasing the non-thermal pressure support has the opposite effect, significantly reducing power at large angular scales. In general, including non-thermal pressure at the level measured in simulations has a large effect on the power spectrum, reducing the amplitude by 50% at angular scales of a few arcminutes compared to a model without a non-thermal component. Our results demonstrate that measurements of the shape of the power spectrum can reveal useful information on important physical processes in groups and clusters, especially at high-redshift where there exists little observational data. Comparing with the recent South Pole Telescope measurements of the small-scale cosmic microwave background power spectrum, we find our model reduces the tension between the values of sigma_8 measured from the SZ power spectrum and from cluster abundances. : 15 Pages, 9 Figures, updated to match version accepted by ApJ |
format |
Text |
author |
Shaw, Laurie D. Nagai, Daisuke Bhattacharya, Suman Lau, Erwin T. |
author_facet |
Shaw, Laurie D. Nagai, Daisuke Bhattacharya, Suman Lau, Erwin T. |
author_sort |
Shaw, Laurie D. |
title |
Impact of Cluster Physics on the Sunyaev-Zel'dovich Power Spectrum |
title_short |
Impact of Cluster Physics on the Sunyaev-Zel'dovich Power Spectrum |
title_full |
Impact of Cluster Physics on the Sunyaev-Zel'dovich Power Spectrum |
title_fullStr |
Impact of Cluster Physics on the Sunyaev-Zel'dovich Power Spectrum |
title_full_unstemmed |
Impact of Cluster Physics on the Sunyaev-Zel'dovich Power Spectrum |
title_sort |
impact of cluster physics on the sunyaev-zel'dovich power spectrum |
publisher |
arXiv |
publishDate |
2010 |
url |
https://dx.doi.org/10.48550/arxiv.1006.1945 https://arxiv.org/abs/1006.1945 |
geographic |
South Pole |
geographic_facet |
South Pole |
genre |
South pole |
genre_facet |
South pole |
op_relation |
https://dx.doi.org/10.1088/0004-637x/725/2/1452 |
op_rights |
arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ |
op_doi |
https://doi.org/10.48550/arxiv.1006.1945 https://doi.org/10.1088/0004-637x/725/2/1452 |
_version_ |
1766202581001961472 |