Phys Rev Lett
SYRTE, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, LNE, 61 avenue de l'Observatoire 75014 Paris, France.
Published: December 2018
We report on a new test of the gravitational redshift and thus of local position invariance, an integral part of the Einstein equivalence principle, which is the foundation of general relativity and all metric theories of gravitation. We use data spanning 1008 days from two satellites of Galileo, Europe's global satellite navigation system, which were launched in 2014, but accidentally delivered on elliptic rather than circular orbits. The resulting modulation of the gravitational redshift of the onboard atomic clocks allows the redshift determination with high accuracy. Additionally, specific laser ranging campaigns to the two satellites have enabled a good estimation of systematic effects related to orbit uncertainties. Together with a careful conservative modeling and control of other systematic effects we measure the fractional deviation of the gravitational redshift from the prediction by general relativity to be (0.19±2.48)×10^{-5} at 1 sigma, improving the best previous test by a factor 5.6. To our knowledge, this represents the first reported improvement on one of the longest standing results in experimental gravitation, the Gravity Probe A hydrogen maser rocket experiment back in 1976.
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http://dx.doi.org/10.1103/PhysRevLett.121.231101 | DOI Listing |
Phys Rev Lett
February 2025
Max Planck Institute for Gravitational Physics, (Albert Einstein Institute) Am Mühlenberg 1, D-14476 Potsdam, Germany.
The ringdown phase following a binary black hole coalescence is a powerful tool for measuring properties of the remnant black hole. Future gravitational wave detectors will increase the precision of these measurements and may be sensitive to the environment surrounding the black hole. This work examines how environments affect the ringdown from a binary coalescence.
View Article and Find Full Text PDFPhys Rev Lett
February 2025
University of California, Riverside, Department of Physics & Astronomy, Riverside, California 92521 USA.
We demonstrate the potential of new adaptive optical technology to expand the detection horizon of gravitational-wave observatories. Achieving greater quantum-noise-limited sensitivity to spacetime strain hinges on achieving higher circulating laser power, in excess of 1 MW, in conjunction with highly squeezed quantum states of light. The new technology will enable significantly higher levels of laser power and squeezing in gravitational-wave detectors, by providing high-precision, low-noise correction of limiting sources of thermal distortions directly to the core interferometer optics.
View Article and Find Full Text PDFPhys Rev Lett
February 2025
University of Modena and Reggio Emilia, Department of Physics, Informatics, and Mathematics, 41125 Modena, Italy.
Observations of massive supermassive black holes (SMBHs) in the early Universe challenge existing black hole formation models. We propose that soliton cores in fuzzy dark matter (FDM) offer a potential solution to this timing problem. Our FDM cosmological zoom-in simulations confirm that, for a particle mass m_{FDM}∼10^{-22} eV, solitons are well developed at redshift z∼7 with masses of ∼10^{9}M_{⊙}, comparable to the observed SMBHs.
View Article and Find Full Text PDFPhys Rev Lett
December 2024
Department of Astronomy, Cornell University, Ithaca, New York 14853, USA.
We present a new perturbative full-shape analysis of BOSS galaxy clustering data, including the full combination of the galaxy power spectrum and bispectrum multipoles, baryon acoustic oscillations, and cross-correlations with the gravitational lensing of cosmic microwave background measured from Planck. Assuming the ΛCDM model, we constrain the matter density fraction Ω_{m}=0.3138±0.
View Article and Find Full Text PDFNat Astron
August 2024
Center for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zurich, Zurich, Switzerland.
The most massive black holes in our Universe form binaries at the centre of merging galaxies. The recent evidence for a gravitational-wave (GW) background from pulsar timing may constitute the first observation that these supermassive black-hole binaries (SMBHBs) merge. Yet, the most massive SMBHBs are out of reach of interferometric GW detectors and are exceedingly difficult to resolve individually with pulsar timing.
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