Testing generalized scalar-tensor theories of gravity with clusters of galaxies

被引：7

作者：

Haridasu, Balakrishna S. ^{[1
,2
,3
]}

Karmakar, Purnendu ^{[4
,5
]}

De Petris, Marco ^{[5
,6
,7
]}

Cardone, Vincenzo F. ^{[6
,7
]}

Maoli, Roberto ^{[5
,6
]}

机构：

[1] SISSA Int Sch Adv Studies, Via Bonomea 265, I-34136 Trieste, Italy

[2] Sez Trieste, INFN, Via Valerio 2, I-34127 Trieste, Italy

[3] Inst Fundamental Phys Universe, IFPU, Via Beirut 2, I-34151 Trieste, Italy

[4] Univ Tokyo, Res Ctr Early Universe RESCEU, Grad Sch Sci, Tokyo 1130033, Japan

[5] Sapienza Univ Roma, Dipartimento Fis, Piazzale Aldo Moro 2, I-00185 Rome, Italy

[6] INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Rome, Italy

[7] Sez Roma 1, INFN, Piazzale Aldo Moro 2, I-00185 Rome, Italy

来源：

PHYSICAL REVIEW D | 2023年 / 107卷 / 12期

关键词：

MASS PROFILES; INTRACLUSTER MEDIUM; THERMODYNAMIC PROPERTIES; SUNYAEV-ZELDOVICH; LAMBDA-CDM; MODELS; ENERGY;

D O I：

10.1103/PhysRevD.107.124059

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We test the generalized scalar tensor theory in static systems, namely galaxy clusters. The degenerate higher-order scalar-tensor (DHOST) theory modifies the Newtonian potential through effective Newtonian constant and 81 parameter in the small scale, which modifies the hydrostatic equilibrium. We utilize the well-compiled X-COP catalog consisting of 12 clusters with intracluster medium (ICM) pressure profile by Sunyaev-Zel'dovich effect data and temperature profile by x-ray data for each cluster. We perform a fully Bayesian analysis modeling Navarro-Frenk-White (NFW) for the mass profile, and the simplified Vikhlinin model for the electron density. Carefully selecting suitable clusters to present our results, we find a mild to moderate, i.e., & SIM;2 & sigma; significance for a deviation from the standard scenario in four of the clusters. However, in terms of Bayesian evidence, we find either equivalent or mild preference for GR. We estimate a joint constraint of 81 = -0.030 & PLUSMN; 0.043 using eight clusters, for a modification from a ?CDM scenario. This limit is in very good agreement with theoretical ones and an order of magnitude more stringent than the previous constraint obtained using clusters. We also quote a more conservative limit of 81 = -0.061 & PLUSMN; 0.074. Finally, we comment on the tentative redshift dependence of the 81 parameter.

引用

页数：17

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