Ultra-light axions and the $S_8$ tension: joint constraints from the cosmic microwave background and galaxy clustering

Abstract

We search for ultra-light axions as dark matter (DM) and dark energy particle candidates, for axion masses $10^{-32}\mathrm{eV}\le m_{\mathrm{a}}\le 10^{-24}\mathrm{eV}$, by a joint analysis of cosmic microwave background (CMB) and galaxy clustering data -- and consider if axions can resolve the tension in inferred values of the matter clustering parameter $S_8$. We give legacy constraints from Planck 2018 CMB data, improving 2015 limits on the axion density ${\Omega }_{\mathrm{a}}{h}^2$ by up to a factor of three; CMB data from the Atacama Cosmology Telescope and the South Pole Telescope marginally weaken Planck bounds at $m_{\mathrm{a}}=10^{-25}\mathrm{eV}$, owing to lower (and theoretically-consistent) gravitational lensing signals. We jointly infer, from Planck CMB and full-shape galaxy power spectrum and bispectrum data from the Baryon Oscillation Spectroscopic Survey (BOSS), that axions are, today, $<10\%$ of the DM for $m_{\mathrm{a}}\le 10^{-26}\mathrm{eV}$ and $<1\%$ for $10^{-30}\mathrm{eV}\le m_{\mathrm{a}}\le 10^{-28}\mathrm{eV}$. BOSS data strengthen limits, in particular at higher $m_{\mathrm{a}}$ by probing high-wavenumber modes ($k<0.4h{\mathrm{Mpc}}^{-1}$). BOSS alone finds a preference for axions at $2.7\sigma$, for $m_{\mathrm{a}}=10^{-26}\mathrm{eV}$, but Planck disfavours this result. Nonetheless, axions in a window $10^{-28}\mathrm{eV}\le m_{\mathrm{a}}\le 10^{-25}\mathrm{eV}$ can improve consistency between CMB and galaxy clustering data, e.g., reducing the $S_8$ discrepancy from $2.7\sigma$ to $1.6\sigma$, since these axions suppress structure growth at the $8h^{-1}\mathrm{Mpc}$ scales to which $S_8$ is sensitive. We expect improved constraints with upcoming high-resolution CMB and galaxy lensing and future galaxy clustering data, where we will further assess if axions can restore cosmic concordance.

53 pages, 22 figures. Minor changes to match version accepted for publication in JCAP

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