Constraints on the Sunyaev-Zel'dovich signal from the Warm Hot Intergalactic Medium from WMAP and SPT data
The fraction of ionized gas in the Warm Hot Intergalactic Medium induces temperature anisotropies on the Cosmic Microwave Background similar to those of clusters of galaxies. The Sunyaev-Zel'dovich anisotropies due to these low density, weakly non-linear, baryon filaments can not be distinguish...
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ftdatacite:10.48550/arxiv.1304.2901 2023-05-15T18:22:52+02:00 Constraints on the Sunyaev-Zel'dovich signal from the Warm Hot Intergalactic Medium from WMAP and SPT data Genova-Santos, Ricardo Suarez-Velasquez, Isabel Atrio-Barandela, Fernando Muecket, Jan 2013 https://dx.doi.org/10.48550/arxiv.1304.2901 https://arxiv.org/abs/1304.2901 unknown arXiv https://dx.doi.org/10.1093/mnras/stt619 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 2013 ftdatacite https://doi.org/10.48550/arxiv.1304.2901 https://doi.org/10.1093/mnras/stt619 2022-04-01T13:24:33Z The fraction of ionized gas in the Warm Hot Intergalactic Medium induces temperature anisotropies on the Cosmic Microwave Background similar to those of clusters of galaxies. The Sunyaev-Zel'dovich anisotropies due to these low density, weakly non-linear, baryon filaments can not be distinguished from that of clusters using frequency information, but they can be separated since their angular scales are very different. To determine the relative contribution of the WHIM SZ signal to the radiation power spectrum of temperature anisotropies, we explore the parameter space of the concordance LCDM model using Monte Carlo Markov Chains and the Wilkinson Microwave Anisotropy Probe 7yr and South Pole Telescope data. We find marginal evidence of a contribution by diffuse gas, with amplitudes of A_WHIM=10-20 muK^2, but the results are also compatible with a null contribution from the WHIM, allowing to set an upper limit of A_WHIM < 43 muK^2 (95.4% C.L.). The signal produced by galaxy clusters remains at A_CL=4.5 muK^2, a value similar to what is obtained when no WHIM is included. From the measured WHIM amplitude we constrain the temperature-density phase diagram of the diffuse gas, and find it to be compatible with numerical simulations. The corresponding baryon fraction in the WHIM varies from 0.43 to 0.47, depending on model parameters. Planck data could set tighter constraints on the temperature-density relation. : Accepted for publication in MNRAS. 9 pages, 5 figures Text South pole DataCite Metadata Store (German National Library of Science and Technology) South Pole Wilkinson ENVELOPE(-66.200,-66.200,-66.817,-66.817) |
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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 |
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Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences Genova-Santos, Ricardo Suarez-Velasquez, Isabel Atrio-Barandela, Fernando Muecket, Jan Constraints on the Sunyaev-Zel'dovich signal from the Warm Hot Intergalactic Medium from WMAP and SPT data |
topic_facet |
Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences |
description |
The fraction of ionized gas in the Warm Hot Intergalactic Medium induces temperature anisotropies on the Cosmic Microwave Background similar to those of clusters of galaxies. The Sunyaev-Zel'dovich anisotropies due to these low density, weakly non-linear, baryon filaments can not be distinguished from that of clusters using frequency information, but they can be separated since their angular scales are very different. To determine the relative contribution of the WHIM SZ signal to the radiation power spectrum of temperature anisotropies, we explore the parameter space of the concordance LCDM model using Monte Carlo Markov Chains and the Wilkinson Microwave Anisotropy Probe 7yr and South Pole Telescope data. We find marginal evidence of a contribution by diffuse gas, with amplitudes of A_WHIM=10-20 muK^2, but the results are also compatible with a null contribution from the WHIM, allowing to set an upper limit of A_WHIM < 43 muK^2 (95.4% C.L.). The signal produced by galaxy clusters remains at A_CL=4.5 muK^2, a value similar to what is obtained when no WHIM is included. From the measured WHIM amplitude we constrain the temperature-density phase diagram of the diffuse gas, and find it to be compatible with numerical simulations. The corresponding baryon fraction in the WHIM varies from 0.43 to 0.47, depending on model parameters. Planck data could set tighter constraints on the temperature-density relation. : Accepted for publication in MNRAS. 9 pages, 5 figures |
format |
Text |
author |
Genova-Santos, Ricardo Suarez-Velasquez, Isabel Atrio-Barandela, Fernando Muecket, Jan |
author_facet |
Genova-Santos, Ricardo Suarez-Velasquez, Isabel Atrio-Barandela, Fernando Muecket, Jan |
author_sort |
Genova-Santos, Ricardo |
title |
Constraints on the Sunyaev-Zel'dovich signal from the Warm Hot Intergalactic Medium from WMAP and SPT data |
title_short |
Constraints on the Sunyaev-Zel'dovich signal from the Warm Hot Intergalactic Medium from WMAP and SPT data |
title_full |
Constraints on the Sunyaev-Zel'dovich signal from the Warm Hot Intergalactic Medium from WMAP and SPT data |
title_fullStr |
Constraints on the Sunyaev-Zel'dovich signal from the Warm Hot Intergalactic Medium from WMAP and SPT data |
title_full_unstemmed |
Constraints on the Sunyaev-Zel'dovich signal from the Warm Hot Intergalactic Medium from WMAP and SPT data |
title_sort |
constraints on the sunyaev-zel'dovich signal from the warm hot intergalactic medium from wmap and spt data |
publisher |
arXiv |
publishDate |
2013 |
url |
https://dx.doi.org/10.48550/arxiv.1304.2901 https://arxiv.org/abs/1304.2901 |
long_lat |
ENVELOPE(-66.200,-66.200,-66.817,-66.817) |
geographic |
South Pole Wilkinson |
geographic_facet |
South Pole Wilkinson |
genre |
South pole |
genre_facet |
South pole |
op_relation |
https://dx.doi.org/10.1093/mnras/stt619 |
op_rights |
arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ |
op_doi |
https://doi.org/10.48550/arxiv.1304.2901 https://doi.org/10.1093/mnras/stt619 |
_version_ |
1766202291659997184 |