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

Haridasu, Balakrishna S.; Karmakar, Purnendu; Petris, M. De; Cardone, V. F.; Maoli, R.

doi:10.48550/arxiv.2111.01101

Cited by 6 publications

(8 citation statements)

References 81 publications

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“…With the exception of the two systems with new observations (A3266 and A2029), we employ the publicly available data products presented in Ghirardini et al (2019) 1 and already used to study the gravitational field of galaxy clusters in several previous works (Ettori et al 2017(Ettori et al , 2019Pradyumna et al 2021;Haridasu et al 2021;Harikumar & Biesiada 2022). Here we briefly recall the data reduction chain developed for X-COP.…”

Section: Xmm-newton Data Analysismentioning

confidence: 99%

The gravitational field of X-COP galaxy clusters

Eckert

Ettori

Pointecouteau

et al. 2022

A&A

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The mass profiles of massive dark matter halos are highly sensitive to the nature of dark matter and potential modifications of the theory of gravity on large scales. The Λ cold dark matter (CDM) paradigm makes strong predictions on the shape of dark matter halos and on the dependence of the shape parameters on halo mass, such that any deviation from the predicted universal shape would have important implications for the fundamental properties of dark matter. Here we use a set of 12 galaxy clusters with available deep X-ray and Sunyaev–Zel’dovich data to constrain the shape of the gravitational field with an unprecedented level of precision over two decades in radius. We introduce a nonparametric framework to reconstruct the shape of the gravitational field under the assumption of hydrostatic equilibrium and compare the resulting mass profiles to the expectations of Navarro–Frenk–White (NFW) and Einasto parametric mass profiles. On average, we find that the NFW profile provides an excellent description of the recovered mass profiles, with deviations of less than 10% over a wide radial range. However, there appears to be more diversity in the shape of individual profiles than can be captured by the NFW model. The average NFW concentration and its scatter agree very well with the prediction of the ΛCDM framework. For a subset of systems, we disentangle the gravitational field into the contribution of baryonic components (gas, brightest cluster galaxy, and satellite galaxies) and that of dark matter. The stellar content dominates the gravitational field inside ∼0.02R500 but is responsible for only 1–2% of the total gravitational field inside R200. The total baryon fraction reaches the cosmic value at R200 and slightly exceeds it beyond this point, possibly indicating a mild level of nonthermal pressure support (10 − 20%) in cluster outskirts. Finally, the relation between observed and baryonic acceleration exhibits a complex shape that strongly departs from the radial acceleration relation in spiral galaxies, which shows that the aforementioned relation does not hold at the galaxy-cluster scale.

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Section: Xmm-newton Data Analysismentioning

confidence: 99%

The gravitational field of X-COP galaxy clusters

Eckert

Ettori

Pointecouteau

et al. 2022

A&A

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“…The study of shocks is highly relevant to cluster-based studies of both cosmology and astrophysics given that they are a critical mechanism during structure formation for converting gravitational potential energy into thermal energy. Shocks can induce significant deviations in cluster pressure profiles, and can set up thermodynamic non-equilibrium conditions that invalidate common assumptions made in estimating hydrostatic cluster masses; these masses are a relevant quantity for doing cosmology with cluster counts (see Allen et al 2011, for a review), while a clear understanding of hydrostatic equilibrium in clusters is necessary for certain clusterbased tests of modified gravity (Terukina et al 2014;Wilcox et al 2015;Sakstein et al 2016;Haridasu et al 2021). Notably, shocks generate a thermal non-equilibrium between the electrons and ions, which can alter the X-ray and tSZ emissions and will consequently need to be considered in analyses that include these cluster outskirts (Fox & Loeb 1997;Ettori & Fabian 1998;Wong & Sarazin 2009;Rudd & Nagai 2009;Akahori & Yoshikawa 2010;Avestruz et al 2015;Vink et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Shocks in the Stacked Sunyaev-Zel'dovich Profiles of Clusters II: Measurements from SPT-SZ + Planck Compton-y Map

Anbajagane,

Chang,

Jain

et al. 2021

Preprint

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We search for the signature of shocks in stacked gas pressure profiles of galaxy clusters using data from the South Pole Telescope (SPT). Specifically, we stack the recently released Compton-𝑦 maps from the 2500 deg 2 SPT-SZ survey on the locations of clusters identified in that same dataset. The sample contains 516 clusters with mean mass 𝑀 200m = 10 14.9 M and redshift 𝑧 = 0.55. We analyze in parallel a set of zoom-in hydrodynamical simulations from T T H project. The SPT-SZ data show two features: (i) a pressure deficit at 𝑅/𝑅 200m = 1.08 ± 0.09, measured at 3.1𝜎 significance and not observed in the simulations, and; (ii) a sharp decrease in pressure at 𝑅/𝑅 200m = 4.58 ± 1.24 at 2.0𝜎 significance. The pressure deficit is qualitatively consistent with a shock-induced thermal non-equilibrium between electrons and ions, and the second feature is consistent with accretion shocks seen in previous studies. We split the cluster sample by redshift and mass, and find both features exist in all cases. There are also no significant differences in features along and across the cluster major axis, whose orientation roughly points towards filamentary structure. As a consistency test, we also analyze clusters from the Planck and Atacama Cosmology Telescope Polarimeter surveys and find quantitatively similar features in the pressure profiles. Finally, we compare the accretion shock radius (𝑅 sh, acc ) with existing measurements of the splashback radius (𝑅 sp ) for SPT-SZ and constrain the lower limit of the ratio, 𝑅 sh, acc /𝑅 sp > 2.16 ± 0.59.

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“…The above bounds are at least one order of magnitude larger than the constraints obtained from stellar probes Jain et al (2016); Babichev et al (2016); Saltas et al (2018); Sakstein (2015aSakstein ( ,b, 2013aSakstein ( ,b, 2018 (see also Koyama & Sakstein (2015b); Sakstein & Koyama (2015)), 2 and than the recent constraints of Haridasu et al (2021) from pressure and temperature profiles of gas in 12 galaxy clusters.…”

Section: Galaxy Kinematics Analysis: Mg-mampossmentioning

confidence: 66%

Probing Vainsthein-screening gravity with galaxy clusters using internal kinematics and strong and weak lensing

Pizzuti,

Saltas,

Umetsu

et al. 2021

Preprint

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We use high-precision combined strong/weak lensing and kinematics measurements of the total mass profiles of the observed galaxy clusters MACS J1206.2-0847 and Abell S1063, to constrain the relativistic sector of the general DHOST dark energy theories, which exhibit a partial breaking of the so called Vainsthein screening mechanism, on the linear level of scalar fluctuations around a cosmological background. In particular, by using the MG-MAMMPOSS framework developed in Pizzuti et al. 2021, for the kinematics analysis of member galaxies in clusters along with lensing mass profile reconstructions we provide new constraints on the coupling 𝑌 2 which governs the theory's relativistic contribution to the lensing potential. The new bound from the combination of kinematics and lensing measurements of MACS 1206, 𝑌 2 = −0.12 +0.66 −0.67 at 2𝜎, provides about a 2-fold improvement on previous constraints. In the case of Abell S1063 a > 2𝜎 tension with the GR expectation arises. We discuss this in some detail, and we investigate the possible sources of systematics which can explain the tension. We further discuss why the combination of kinematics of member galaxies with lensing is capable of providing much tighter bounds compared to kinematics or lensing alone, and we explain how the number density profile of tracers, as well as the choice of the velocity anisotropy profile affects the final results.

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

Cited by 6 publications

References 81 publications

The gravitational field of X-COP galaxy clusters

The gravitational field of X-COP galaxy clusters

Shocks in the Stacked Sunyaev-Zel'dovich Profiles of Clusters II: Measurements from SPT-SZ + Planck Compton-y Map

Probing Vainsthein-screening gravity with galaxy clusters using internal kinematics and strong and weak lensing

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