Mass Modeling and Kinematics of Galaxy Clusters in Modified Gravity
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arXiv
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| Main Authors: | , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866909390408253440 |
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| author | Pizzuti, Lorenzo Boumechta, Yacer Haridasu, Sandeep Pombo, Alexandre M. Dossena, Sofia Butt, Minahil Adil Benetti, Francesco Baccigalupi, Carlo Lapi, Andrea |
| author_facet | Pizzuti, Lorenzo Boumechta, Yacer Haridasu, Sandeep Pombo, Alexandre M. Dossena, Sofia Butt, Minahil Adil Benetti, Francesco Baccigalupi, Carlo Lapi, Andrea |
| contents | The chameleon screening mechanism has been constrained many a time using dynamic and kinematic galaxy cluster observables. Current constraints are, however, insensitive to different mass components within galaxy clusters and have been mainly focused on a single mass density profile, the Navarro-Frenk-While mass density model. In this work, we extend the study of the Chameleon screening mechanism in galaxy clusters by considering a series of mass density models, namely: generalized-Navarro-Frenk-While, b-Navarro-Frenk-While, Burket, Isothermal and Einasto. The coupling strength ($β$) and asymptotic value of the chameleon field ($ϕ_\infty$) are constrained by using kinematics analyses of simulated galaxy clusters, generated both assuming General Relativity and a strong chameleon scenario. By implementing a Bayesian analysis we comprehensively show that the biases introduced due to an incorrect assumption of the mass model are minimal. Similarly, we also demonstrate that a spurious detection of evidence for modifications to gravity is highly unlikely when utilizing the kinematics of galaxy clusters. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2407_08778 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Mass Modeling and Kinematics of Galaxy Clusters in Modified Gravity Pizzuti, Lorenzo Boumechta, Yacer Haridasu, Sandeep Pombo, Alexandre M. Dossena, Sofia Butt, Minahil Adil Benetti, Francesco Baccigalupi, Carlo Lapi, Andrea Cosmology and Nongalactic Astrophysics The chameleon screening mechanism has been constrained many a time using dynamic and kinematic galaxy cluster observables. Current constraints are, however, insensitive to different mass components within galaxy clusters and have been mainly focused on a single mass density profile, the Navarro-Frenk-While mass density model. In this work, we extend the study of the Chameleon screening mechanism in galaxy clusters by considering a series of mass density models, namely: generalized-Navarro-Frenk-While, b-Navarro-Frenk-While, Burket, Isothermal and Einasto. The coupling strength ($β$) and asymptotic value of the chameleon field ($ϕ_\infty$) are constrained by using kinematics analyses of simulated galaxy clusters, generated both assuming General Relativity and a strong chameleon scenario. By implementing a Bayesian analysis we comprehensively show that the biases introduced due to an incorrect assumption of the mass model are minimal. Similarly, we also demonstrate that a spurious detection of evidence for modifications to gravity is highly unlikely when utilizing the kinematics of galaxy clusters. |
| title | Mass Modeling and Kinematics of Galaxy Clusters in Modified Gravity |
| topic | Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2407.08778 |