Abstract
Astrophysical tests of current values for dimensionless constants known on Earth, such as the fine-structure constant, α , and proton-to-electron mass ratio, μ = m p / m e , are communicated using data from high-resolution quasar spectra in different regions or epochs of the universe. The symmetry wavelengths of [Fe II] lines from redshifted quasar spectra of J110325-264515 and their corresponding values in the laboratory were combined to find a new limit on space-time variations in the proton-to-electron mass ratio, ∆ μ / μ = ( 0.096 ± 0.182 ) × 10 − 7 . The results show how the indicated astrophysical observations can further improve the accuracy and space-time variations of physics constants.
Highlights
IntroductionUsing new sources at current and future detectors allows us to indicate non-General Relativity (GR) effects that help us better understand the important relation
A motivating challenge is related to varying dimensionless physics constants for example, the fine-structure constant, α = 4πεe }c, and the ratio of proton-to-electron mass ratio, μ = mp /me.This continues to be an interesting problem in both experimental and theoretical physics phenomena for the validation of the Standard Model (SM) [1,2,3,4,5] because values and dependence on parameters over the cosmological timescales of α and μ values have not been explained or predicted by the SM.variations of these constants over cosmological time or space would violate the EinsteinEquivalence Principle (EEP), which is the basic assumption of General Relativity (GR)
On the basis of the tests passed with flying colors, the deviations of GR would only be predicted at some lengths or energy scales [6,7,8]
Summary
Using new sources at current and future detectors allows us to indicate non-GR effects that help us better understand the important relation This has been a motivator for astrophysical and cosmological studies beyond GR without including dark energy or dark matter, as it is used for explaining the present accelerating and expanding universe and other interesting problems in galaxies such as missing mass. The most important of these are the accuracy of the wavelength calibrations, assumptions of uniform velocity structure, and uniform spatial abundance patterns in [Fe II] lines In this way, the advantage of this procedure and the fitting procedure is that they can determine ∆α/α with higher precision than the previous results. Based on existing astrophysical observations of [Fe II] in absorption systems, we identified the variation of the proton-to-electron mass ratio in our galaxy, and provide significant improvement for future astrophysical measurements of higher precision to more stringently test whether the ∆α/α and ∆μ/μ vary
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