Testing general relativity with present and future astrophysical observations

Berti, Emanuele; Barausse, Enrico; Cardoso, Vítor; Gualtieri, Leonardo; Pani, Paolo; Sperhake, Ulrich; Stein, Leo C.; Wex, Norbert; Yagi, Kent; Baker, Tessa; Burgess, C. P.; Coelho, Flávio S.; Doneva, Daniela D.; Felice, Antonio De; Ferreira, Pedro G.; Freire, P. C. C.; Healy, J.; Herdeiro, Carlos; Horbatsch, Michael; Kleihaus, Burkhard; Klein, Antoine; Kokkotas, Kostas D.; Kunz, Jutta; Laguna, Pablo; Lang, R. N.; Li, Tjonnie G. F.; Littenberg, T. B.; Matas, A.; Mirshekari, S.; Okawa, Hirotada; Radu, Eugen; O’Shaughnessy, R.; Sathyaprakash, B. S.; Broeck, C. Van Den; Winther, Hans A.; Witek, Helvi; Aghili, Mir Emad; Alsing, Justin; Bolen, Brett; Bombelli, L.; Caudill, S.; Chen, Liang; Degollado, Juan Carlos; Fujita, Ryuichi; Gao, Caixia; Gerosa, Davide; Kamali, Saeed; Silva, Hector O.; Rosa, João G.; Sadeghian, L.; Sampaio, Marco O. P.; Sotani, Hajime; Zilhão, Miguel

doi:10.1088/0264-9381/32/24/243001

Cited by 1,324 publications

(1,391 citation statements)

References 884 publications

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“…Many summaries of existing and prospective tests of gravity were written prior to the gravitational wave event; some recent examples that we recommend are [61,62,63,59] . There has also been detailed analysis of the implications of GW150914 itself for gravitational physics [64,65].…”

Section: Implications For Gravitational Physicsmentioning

confidence: 99%

Implications of the gravitational wave event GW150914

Miller

2016

Gen Relativ Gravit

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The era of gravitational-wave astronomy began on 14 September 2015, when the LIGO Scientific Collaboration detected the merger of two ∼ 30 M ⊙ black holes at a distance of ∼ 400 Mpc. This event has facilitated qualitatively new tests of gravitational theories, and has also produced exciting information about the astrophysical origin of black hole binaries. In this review we discuss the implications of this event for gravitational physics and astrophysics, as well as the expectations for future detections. In brief: (1) because the spins of the black holes could not be measured accurately and because mergers are not well calculated for modified theories of gravity, the current analysis of GW150914 does not place strong constraints on gravity variants that change only the generation of gravitational waves, but (2) it does strongly constrain alterations of the propagation of gravitational waves and alternatives to black holes. Finally, (3) many astrophysical models for the origin of heavy black hole binaries such as the GW150914 system are in play, but a reasonably robust conclusion that was reached even prior to the detection is that the environment of such systems needs to have a relatively low abundance of elements heavier than helium.

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Section: Implications For Gravitational Physicsmentioning

confidence: 99%

Implications of the gravitational wave event GW150914

Miller

2016

Gen Relativ Gravit

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“…The screening can be accomplished in many ways [19,60]: with a weak coupling between the field and matter in regions of high density, thus inducing a weak fifth-force as in symmetron theories [52,53]; the field can acquire a large mass in high density environments, being short-ranged and undetectable, and be light and long-ranged in lower density regions, as for chameleon fields [20,61,62,75,76] and f (R) models [27,28,36,96]; or one may change the kinetic contribution of the field to the Lagrangian, with first or second order derivatives becoming important in a certain range, as it happens with the Vainshtein screening mechanism [101].…”

Section: Introductionmentioning

confidence: 99%

Breaking the Vainshtein screening in clusters of galaxies

et al. 2017

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In this work we will test an alternative model of gravity belonging to the large family of galileon models. It is characterized by an intrinsic breaking of the Vainshtein mechanism inside large astrophysical objects, thus having possibly detectable observational signatures. We will compare theoretical predictions from this model with the observed total mass profile for a sample of clusters of galaxies. The profiles are derived using two complementary tools: X-ray hot intra-cluster gas dynamics, and strong and weak gravitational lensing. We find that a dependence with the dynamical internal status of each cluster is possible; for those clusters which are very close to be relaxed, and thus less perturbed by possible astrophysical local processes, the galileon model gives a quite good fit to both X-ray and lensing observations. Both masses and concentrations for the dark matter halos are consistent with earlier results found in numerical simulations and in the literature, and no compelling statistical evidence for a deviation from general relativity is detectable from the present observational state. Actually, the characteristic galileon parameter Υ is always consistent with zero, and only an upper limit ( 0.086 at 1σ, 0.16 at 2σ, and 0.23 at 3σ) can be established. Some interesting distinctive deviations might be operative, but the statistical validity of the results is far from strong, and better data would be needed in order to either confirm or reject a potential tension with general relativity.PACS numbers: 04.50. Kd, 98.80.Es, 95.35. + d

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“…For more details on the implementation of the scalar fields and other technicalities we refer to . For this purpose, we focus on simple observables such as the matter power spectrum, halo mass function, density profiles, and velocity profiles to investigate modified gravity signatures that were previously studied in Li et al (2012bLi et al ( , 2013, Hammami et al (2015), Schmidt et al (2009), Gronke et al (2015, Lombriser et al (2012Lombriser et al ( , 2014, Winther et al (2012), Terukina & Yamamoto (2012), Shi et al (2015), Pujol et al (2014), Hellwing et al (2013), He et al (2013He et al ( , 2015, Schmidt (2010), Brax et al (2013), Tessore et al (2015), Gronke et al (2015) that can also be observed (Berti et al 2015;Zivick et al 2015;Mak et al 2012;Cai et al 2015;Song et al 2015;Wilcox et al 2015;Jain & Khoury 2010;Schmidt 2010;Hellwing et al 2014). This paper is organized as follows: in Sect.…”

Section: Introductionmentioning

confidence: 99%

N-body simulations ofγgravity

Santos

Winther

Mota

et al. 2016

A&A

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We have investigated structure formation in the γ gravity f (R) model with N-body simulations. The γ gravity model is a proposal which, unlike other viable f (R) models, not only changes the gravitational dynamics, but can in principle also have signatures at the background level that are different from those obtained in ΛCDM (Cosmological constant, Cold Dark Matter). The aim of this paper is to study the nonlinear regime of the model in the case where, at late times, the background differs from ΛCDM. We quantify the signatures produced on the power spectrum, the halo mass function, and the density and velocity profiles. To appreciate the features of the model, we have compared it to ΛCDM and the Hu-Sawicki f (R) models. For the considered set of parameters we find that the screening mechanism is ineffective, which gives rise to deviations in the halo mass function that disagree with observations. This does not rule out the model per se, but requires choices of parameters such that | f R0 | is much smaller, which would imply that its cosmic expansion history cannot be distinguished from ΛCDM at the background level.

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Testing general relativity with present and future astrophysical observations

Cited by 1,324 publications

References 884 publications

Implications of the gravitational wave event GW150914

Implications of the gravitational wave event GW150914

Breaking the Vainshtein screening in clusters of galaxies

N-body simulations ofγgravity

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