Cosmic Birefringence Test of the Hubble Tension

Abstract

An early dark energy component consisting of a cosmic pseudo Nambu-Goldstone boson has been recently proposed to resolve the Hubble tension -- the four-sigma discrepancy between precision measurements of the expansion rate of the universe. Here we point out that such an axion-like component may be expected to couple to electromagnetism by a Chern-Simons term, and will thereby induce an anisotropic cosmic birefringence signal in the polarization of the cosmic microwave background (CMB). We show that observations of the rotation-angle power spectrum and cross-correlation with CMB temperature anisotropy can confirm the presence of this early dark energy component. Future CMB data as expected from the CMB-S4 experiment will improve sensitivity to this effect by two orders of magnitude and help in discriminating between different Hubble tension scenarios.

6 pages, 2 figures

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• Neutrino-Assisted Early Dark Energy: Theory and Cosmology
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• Probing Axion-like Particles via CMB Polarization
• Cosmological implications of $n_s\approx 1$ in light of the Hubble tension
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• Probing Axions through Tomography of Anisotropic Cosmic Birefringence
• CMB Mode Coupling with Isotropic Polarization Rotation
• Bayesian analysis of a Unified Dark Matter model with transition: can it alleviate the $H_0$ tension?
• A New Solution for the Observed Isotropic Cosmic Birefringence Angle and its Implications for the Anisotropic Counterpart through a Boltzmann Approach
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• Impact of Anisotropic Birefringence on Measuring Cosmic Microwave Background Lensing
• Computing Microwave Background Polarization Power Spectra from Cosmic Birefringence
• Breaking parity: the case of the trispectrum from chiral scalar-tensor theories of gravity
• Conversations in the dark: cross-correlating birefringence and LSS to constrain axions
• Polarization Calibration of a Microwave Polarimeter with Near-Infrared Up-Conversion for Optical Correlation and Detection
• The cosmological evolution of ultralight axionlike scalar fields
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