Constraining the mass and redshift evolution of the hydrostatic mass bias using the gas mass fraction in galaxy clusters
The gas mass fraction in galaxy clusters is a quantity which can be used as a robust cosmological probe. It is however subject to various effects from the baryonic physics inside galaxy clusters, which may bias the obtained cosmological constraints. Among different aspects of the baryonic physics, i...
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| Format: | Article |
| Language: | English |
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EDP Sciences
2024-01-01
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| Series: | EPJ Web of Conferences |
| Online Access: | https://www.epj-conferences.org/articles/epjconf/pdf/2024/03/epjconf_mmUniverse2023_00052.pdf |
| _version_ | 1797235277131939840 |
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| author | Wicker R. Douspis M. Salvati L. Aghanim N. |
| author_facet | Wicker R. Douspis M. Salvati L. Aghanim N. |
| author_sort | Wicker R. |
| collection | DOAJ |
| description | The gas mass fraction in galaxy clusters is a quantity which can be used as a robust cosmological probe. It is however subject to various effects from the baryonic physics inside galaxy clusters, which may bias the obtained cosmological constraints. Among different aspects of the baryonic physics, in these proceedings we focus on the impact of the hydrostatic equilibrium assumption. From X-ray measurements of cluster gas fraction in the Planck-ESZ sample, we analyse the hydrostatic mass bias B, constraining a possible mass and redshift evolution of this quantity and its impact on the cosmological constraints. We show a degeneracy between the redshift dependence of the bias and cosmological parameters. In particular we find a 3.8σ evidence for a redshift dependence of the bias when assuming a Planck prior on Ωm. On the other hand, assuming a constant mass bias would lead to the extreme large value of Ωm > 0.860. We however show these results to be depending on the mass and redshift selections inside the main sample. Nevertheless, in all the analyses we find a value for the amplitude of the bias that is consistent with B ∼ 0.8, as expected from hydrodynamical simulations and local measurements, but still in tension with the low value of B ∼ 0.6 derived from the combination of cosmic microwave background primary anisotropies with cluster number counts. We also discuss cosmological constraints obtained from gas fraction data, combined with other probes like cluster number counts. |
| first_indexed | 2024-04-24T16:45:24Z |
| format | Article |
| id | doaj.art-bc25dd58bd7a4ef393c782c978ebfaae |
| institution | Directory Open Access Journal |
| issn | 2100-014X |
| language | English |
| last_indexed | 2024-04-24T16:45:24Z |
| publishDate | 2024-01-01 |
| publisher | EDP Sciences |
| record_format | Article |
| series | EPJ Web of Conferences |
| spelling | doaj.art-bc25dd58bd7a4ef393c782c978ebfaae2024-03-29T08:31:01ZengEDP SciencesEPJ Web of Conferences2100-014X2024-01-012930005210.1051/epjconf/202429300052epjconf_mmUniverse2023_00052Constraining the mass and redshift evolution of the hydrostatic mass bias using the gas mass fraction in galaxy clustersWicker R.0Douspis M.1Salvati L.2Aghanim N.3Université Paris-Saclay, CNRS, Institut d’Astrophysique SpatialeUniversité Paris-Saclay, CNRS, Institut d’Astrophysique SpatialeUniversité Paris-Saclay, CNRS, Institut d’Astrophysique SpatialeUniversité Paris-Saclay, CNRS, Institut d’Astrophysique SpatialeThe gas mass fraction in galaxy clusters is a quantity which can be used as a robust cosmological probe. It is however subject to various effects from the baryonic physics inside galaxy clusters, which may bias the obtained cosmological constraints. Among different aspects of the baryonic physics, in these proceedings we focus on the impact of the hydrostatic equilibrium assumption. From X-ray measurements of cluster gas fraction in the Planck-ESZ sample, we analyse the hydrostatic mass bias B, constraining a possible mass and redshift evolution of this quantity and its impact on the cosmological constraints. We show a degeneracy between the redshift dependence of the bias and cosmological parameters. In particular we find a 3.8σ evidence for a redshift dependence of the bias when assuming a Planck prior on Ωm. On the other hand, assuming a constant mass bias would lead to the extreme large value of Ωm > 0.860. We however show these results to be depending on the mass and redshift selections inside the main sample. Nevertheless, in all the analyses we find a value for the amplitude of the bias that is consistent with B ∼ 0.8, as expected from hydrodynamical simulations and local measurements, but still in tension with the low value of B ∼ 0.6 derived from the combination of cosmic microwave background primary anisotropies with cluster number counts. We also discuss cosmological constraints obtained from gas fraction data, combined with other probes like cluster number counts.https://www.epj-conferences.org/articles/epjconf/pdf/2024/03/epjconf_mmUniverse2023_00052.pdf |
| spellingShingle | Wicker R. Douspis M. Salvati L. Aghanim N. Constraining the mass and redshift evolution of the hydrostatic mass bias using the gas mass fraction in galaxy clusters EPJ Web of Conferences |
| title | Constraining the mass and redshift evolution of the hydrostatic mass bias using the gas mass fraction in galaxy clusters |
| title_full | Constraining the mass and redshift evolution of the hydrostatic mass bias using the gas mass fraction in galaxy clusters |
| title_fullStr | Constraining the mass and redshift evolution of the hydrostatic mass bias using the gas mass fraction in galaxy clusters |
| title_full_unstemmed | Constraining the mass and redshift evolution of the hydrostatic mass bias using the gas mass fraction in galaxy clusters |
| title_short | Constraining the mass and redshift evolution of the hydrostatic mass bias using the gas mass fraction in galaxy clusters |
| title_sort | constraining the mass and redshift evolution of the hydrostatic mass bias using the gas mass fraction in galaxy clusters |
| url | https://www.epj-conferences.org/articles/epjconf/pdf/2024/03/epjconf_mmUniverse2023_00052.pdf |
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