Tests of general relativity

Summary

Tests of general relativity serve to establish observational evidence for the theory of general relativity. The first three tests, proposed by Albert Einstein in 1915, concerned the "anomalous" precession of the perihelion of Mercury, the bending of light in gravitational fields, and the gravitational redshift. The precession of Mercury was already known; experiments showing light bending in accordance with the predictions of general relativity were performed in 1919, with increasingly precise measurements made in subsequent tests; and scientists claimed to have measured the gravitational redshift in 1925, although measurements sensitive enough to actually confirm the theory were not made until 1954. A more accurate program starting in 1959 tested general relativity in the weak gravitational field limit, severely limiting possible deviations from the theory. In the 1970s, scientists began to make additional tests, starting with Irwin Shapiro's measurement of the relativistic time dela

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https://en.wikipedia.org/wiki/Tests_of_general_relativity

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Comparison of Einstein-Boltzmann solvers for testing general relativity

Mikhail Ivanov, Bing Li

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Testing general relativity on cosmological scales at redshift z similar to 1.5 with quasar and CMB lensing

Cheng Zhao

We test general relativity (GR) at the effective redshift (z) over tilde similar to 1.5 by estimating the statistic E-G, a probe of gravity, on cosmological scales 19 - 190 h(-1)Mpc. This is the highest redshift and largest scale estimation of E-G so far. We use the quasar sample with redshifts 0.8 < z < 2.2 from Sloan Digital Sky Survey IV extended Baryon Oscillation Spectroscopic Survey Data Release 16 as the large-scale structure (LSS) tracer, for which the angular power spectrum C-l(qq) and the redshift-space distortion parameter beta are estimated. By cross-correlating with the Planck 2018 cosmic microwave background (CMB) lensing map, we detect the angular cross-power spectrum Cl-kappa q signal at 12 sigma significance. Both jackknife resampling and simulations are used to estimate the covariance matrix (CM) of E-G at five bins covering different scales, with the later preferred for its better constraints on the covariances. We find E-G estimates agree with the GR prediction at 1 sigma level over all these scales. With the CM estimated with 300 simulations, we report a best-fitting scale-averaged estimate of E-G((z) over bar) = 0.30 +/- 0.05, which is in line with the GR prediction E-G(GR)((z) over bar) = 0.33 with Planck 2018 CMB + BAO matter density fraction Omega(m) = 0.31. The statistical errors of E-G with future LSS surveys at similar redshifts will be reduced by an order of magnitude, which makes it possible to constrain modified gravity models.

OXFORD UNIV PRESS2021