Axion-like Dark Matter Constraints from CMB Birefringence

TL;DR

This paper uses measurements of cosmic microwave background birefringence to set new, stringent constraints on axion-like dark matter particles' properties, significantly improving previous limits and guiding future research.

Contribution

It introduces a novel method to constrain ultra-light axion-like particles using CMB birefringence, achieving up to four orders of magnitude improvement over prior bounds.

Findings

Constraints on axion-photon coupling: g_{aγ} ≲ 10^{-17}–10^{-12} GeV^{-1}

Limits on ALP mass range: 10^{-27}–10^{-24} eV

Potential for future CMB observations to further tighten constraints

Abstract

Axion-like particles are dark matter candidates motivated by the Peccei-Quinn mechanism and also occur in effective field theories where their masses and photon couplings are independent. We estimate the dispersion of circularly polarized photons in a background of oscillating axion-like particles (ALPs) with the standard $g_{a\gamma}\,a\,F_{\mu\nu}\tilde F^{\mu\nu}/4$ coupling to photons. This leads to birefringence or rotation of linear polarization by ALP dark matter. Cosmic microwave background (CMB) birefringence limits $\Delta \alpha \lesssim (1.0)^\circ$ enable us to constrain the axion-photon coupling $g_{a\gamma} \lesssim 10^{-17}-10^{-12}\,{\rm GeV}^{-1}$, for ultra-light ALP masses $m_a \sim 10^{-27} - 10^{-24}$ eV. This improves upon previous axion-photon coupling limits by up to four orders of magnitude. Future CMB observations could tighten limits by another one to two orders.