Gravitational Test beyond the First Post-Newtonian Order with the Shadow of the M87 Black Hole

Psaltis, Dimitrios; Medeiros, Lia; Christian, Pierre; Özel, Feryal; Akiyama, Kazunori; Alberdi, A.; Alef, W.; Asada, Keiichi; Azulay, Rebecca; Ball, D. R.; Baloković, Mislav; Barrett, John; Bintley, Dan; Blackburn, L.; Boland, W.; Bower, Geoffrey C.; Bremer, M.; Brinkerink, Christiaan D.; Brissenden, Roger; Britzen, S.; Broguière, Dominique; Bronzwaer, Thomas; Byun, Doyoung; Carlstrom, J. E.; Chael, Andrew; Chan, Chi-kwan; Chatterjee, Shami; Chatterjee, Koushik; Chen, Ming-Tang; Chen, Yongjun; Cho, Ilje; Conway, J.; Cordes, J. M.; Crew, G. B.; Cui, Yuzhu; Davelaar, Jordy; Laurentis, Mariafelicia De; Deane, Roger; Dempsey, Jessica; Desvignes, G.; Dexter, Jason; Eatough, Ralph P.; Falcke, H.; Fish, Vincent L.; Fomalont, Ed; Fraga-Encinas, Raquel; Friberg, Per; Fromm, Christian M.; Gammie, Charles F.; Garcı́a, Roberto; Gentaz, Olivier; Goddi, C.; Gómez, J. L.; Gu, Minfeng; Gurwell, M. A.; Hada, Kazuhiro; Hesper, Ronald; Ho, Luis C.; Ho, Paul T. P.; Honma, Mareki; Huang, Chih-Wei L.; Huang, Lei; Hughes, D. H.; Inoue, Makoto; Issaoun, Sara; James, D. J.; Jannuzi, Buell T.; Janssen, Michaël; Jiang, Wu; Jiménez-Rosales, A.; Johnson, Michael D.; Jorstad, Svetlana G.; Jung, Taehyun; Karami, Mansour; Karuppusamy, R.; Kawashima, Tomohisa; Keating, Garrett K.; Kettenis, Mark; Kim, Jae‐Young; Kim, Junhan; Kim, Jong-Soo; Kino, Motoki; Koay, Jun Yi; Koch, Patrick M.; Koyama, Shoko; Krämer, M.; Krämer, C.; Krichbaum, T. P.; Kuo, Cheng‐Yu; Lauer, Tod R.; Lee, Sang-Sung; Li, Yanrong; Li, Zhiyuan; Lindqvist, Michael; Lico, Rocco; Li, Jun; Li, Kuo; Liuzzo, E.; Lo, Wen-Ping; Lobanov, A. P.; Lonsdale, Colin J.; Lu, Ru-Sen; Mao, Jirong; Markoff, Sera; Marrone, Daniel P.; Marscher, A. P.; Martí-Vidal, Iván; Matsushita, Satoki; Mizuno, Yosuke; Mizuno, Izumi; Moran, J. M.; Moriyama, Kotaro; Mościbrodzka, Monika; Müller, C.; Musoke, Gibwa; Mus, Alejandro; Nagai, Hiroshi; Nagar, Neil M.; Narayan, Ramesh; Narayanan, Gopal; Natarajan, Iniyan; Neri, R.; Noutsos, A.; Okino, Hiroki; Olivares, Héctor; Oyama, Tomoaki; Palumbo, Daniel C. M.; Park, Jong Ho; Patel, Nimesh; Pen, Ue-Li; Piétu, V.; Plambeck, R. L.; PopStefanija, Aleksandar; Prather, Ben; Preciado-López, Jorge A.; Ramakrishnan, Venkatessh; Rao, Ramprasad; Rawlings, Mark G.; Raymond, Alexander W.; Ripperda, Bart; Roelofs, Freek; Rogers, A. E. E.; Ros, E.; Rose, Mel; Roshanineshat, Arash; Rottmann, Helge; Roy, A. L.; Ruszczyk, Chet; Ryan, Benjamin R.; Rygl, K. L. J.; Sánchez, Salvador; Sánchez-Argüelles, David; Sasada, Mahito; Savolainen, Tuomas; Schloerb, F. Peter; Schüster, K.; Shao, Lijing; Shen, Zhi-Qiang; Small, Des; Sohn, Bong Won; Soohoo, Jason; Tazaki, Fumie; Tilanus, R. P. J.; Titus, Michael S.; Torné, Pablo; Trent, Tyler; Traianou, Efthalia; Trippe, Sascha; Bemmel, Ilse van; Langevelde, H. J. van; Rossum, Daniel R. van; Wagner, Jan; Wardle, J. F. C.; Ward-Thompson, Derek; Weintroub, Jonathan; Wex, Norbert; Wharton, Robert; Wielgus, Maciek; Wong, George N.; Wu, Qingwen; Yoon, Doosoo; Young, André; Young, Ken; Younsi, Ziri; Yuan, Feng; Yuan, Ye‐Fei; Zhao, Shan-Shan

doi:10.1103/physrevlett.125.141104

Cited by 230 publications

(204 citation statements)

References 56 publications

(56 reference statements)

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“…[82] was done under the assumption of spherically symmetric BHs, which certainly will not be valid for all the gravitational wave events, and the inclusion of spin will worsen the estimates there. Another recent work [83] uses the results from the observation of the supermassive BH at the center of the M87 galaxy, reported by the Event Horizon Telescope collaboration [11], to place constraints on the leading order strong-gravity deformation parameter, which is the same as our δ 1 . The constraints obtained there are a few times weaker than those reported here.…”

Section: Discussionmentioning

confidence: 99%

Testing general relativity with x-ray reflection spectroscopy: The Konoplya-Rezzolla-Zhidenko parametrization

et al. 2020

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X-ray reflection spectroscopy is a promising technique for testing general relativity in the strong-field regime as it can be used to test the Kerr black hole hypothesis. In this context, the parametrically deformed black hole metrics proposed by Konoplya, Rezzolla, and Zhidenko [Phys. Rev. D 93, 064015 (2016)] form an important class of non-Kerr black holes. We implement this class of black hole metrics in RELXILL_NK, which is a framework we have developed for testing for non-Kerr black holes using x-ray reflection spectroscopy. We perform a qualitative analysis of the effect of the leading order strong-field deformation parameters on typical observables like the innermost stable circular orbits and the reflection spectra. We also present the first x-ray constraints on some of the deformation parameters of this metric, using Suzaku data from the supermassive black hole in Ark 564, and compare them with those obtained (or expected) from other observational techniques like gravitational waves and black hole imaging.

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Section: Discussionmentioning

confidence: 99%

Testing general relativity with x-ray reflection spectroscopy: The Konoplya-Rezzolla-Zhidenko parametrization

et al. 2020

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“…Moreover, proofs of concept of the feasibility of testing general relativity, or even the existence of new particles via EHT observations have been reported in, e.g. [13][14][15][16][17][18][19].…”

Section: Introductionmentioning

confidence: 99%

Magnetized accretion disks around Kerr black holes with scalar hair: Constant angular momentum disks

et al. 2019

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Testing the true nature of black holes -the no-hair hypothesis -will become increasingly more precise in the next few years as new observational data is collected in both the gravitational wave channel and the electromagnetic channel. In this paper we consider numerically generated spacetimes of Kerr black holes with synchronised scalar hair and build stationary models of magnetized thick disks (or tori) around them. Our approach assumes that the disks are not self-gravitating, they obey a polytropic equation of state, the distribution of their specific angular momentum is constant, and they are marginally stable, i.e. the disks completely fill their Roche lobe. Moreover, contrary to existing approaches in the literature, our models are thermodinamically relativist, as the specific enthalpy of the fluid can adopt values significantly larger than unity. We study the dependence of the morphology and properties of the accretion tori on the type of black hole considered, from purely Kerr black holes with varying degrees of spin parameter, namely from a Schwarzschild black hole to a nearly extremal Kerr case, to Kerr black holes with scalar hair with different ADM mass and horizon angular velocity. Comparisons between the disk properties for both types of black holes are presented. The sequences of magnetized, equilibrium disks models discussed in this study can be used as initial data for numerical relativity codes to investigate their dynamical (non-linear) stability and used in tandem with ray-tracing codes to obtain synthetic images of black holes (i.e. shadows) in astrophysically relevant situations where the light source is provided by an emitting accretion disk.PACS numbers: 95.30. Sf, 04.70.Bw, 04.25.dg 95.30.Qd

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“…forming with the Weyl tensor C αβγδ and the NP tetrad (21). As we will see, in short, these quantities correspond to the odd (axial) gravitational perturbation of Ref.…”

Section: Basic Equations and Separation Of Variablesmentioning

confidence: 88%

“…Due to the EHT activity it is believed more and more that Astrophysical BHs (BHs in the sky) share common properties with mathematical BHs (solutions to Einstein equations). • Last but not least: the recent data analysis of the EHT team puts the Einstein theory on the test [21]. It turns out that general relativity works well, and many alternative theories of gravity should be discarded as that of contradicting experimental data.…”

Section: Introductionmentioning

confidence: 99%

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Scattering on Quasi-Spherical Black-Holes: Features and Beyond

Arslanaliev

Nurmagambetov

2021

Physics

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Recent developments in the gravitational waves interferometry require more pertinent theoretical models of gravitational waves generation and propagation. Untouched possible mechanisms of spin-2 spacetime perturbations production, we will consider their subsequent scattering on other black holes (BHs). Specifically, we consider a generalization of the Regge-Wheeler-Zerilli equations for the case of distorted BHs (BHs surrounded with matter) in Minkowski and Anti-de Sitter spacetimes, the metric potential of which obeys the Liouville equation. We establish significant differences in scattering characteristics of waves of different spins and angular momenta, including the gravitational waves, caused by losing the spherical symmetry of their propagation background. In particular, we demonstrate the strong impact of the background geometry deformation on the grey-body factors, hence on the absorption cross-sections of scattering waves, and explore the issue of stability of the background geometry upon changing the deformation degree parameters.

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Gravitational Test beyond the First Post-Newtonian Order with the Shadow of the M87 Black Hole

Cited by 230 publications

References 56 publications

Testing general relativity with x-ray reflection spectroscopy: The Konoplya-Rezzolla-Zhidenko parametrization

Testing general relativity with x-ray reflection spectroscopy: The Konoplya-Rezzolla-Zhidenko parametrization

Magnetized accretion disks around Kerr black holes with scalar hair: Constant angular momentum disks

Scattering on Quasi-Spherical Black-Holes: Features and Beyond

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