Future CMB tests of dark matter: ultra-light axions and massive neutrinos

Abstract

Measurements of cosmic microwave background (CMB) anisotropies provide strong evidence for the existence of dark matter and dark energy. They can also test its composition, probing the energy density and particle mass of different dark-matter and dark-energy components. CMB data have already shown that ultra-light axions (ULAs) with mass in the range $10^{-32}\mathrm{eV}\to 10^{-26}\mathrm{eV}$ compose a fraction $<0.01$ of the cosmological critical density. Here, the sensitivity of a proposed CMB-Stage IV (CMB-S4) experiment (assuming a 1 arcmin beam and $<1\mu K-\mathrm{arcmin}$ noise levels over a sky fraction of 0.4) to the density of ULAs and other dark-sector components is assessed. CMB-S4 data should be $\sim 10$ times more sensitive to the ULA energy-density than Planck data alone, across a wide range of ULA masses $10^{-32}<m_a<10^{-23}\mathrm{eV}$, and will probe axion decay constants of $f_a\approx 10^{16}\mathrm{GeV}$, at the grand unified scale. CMB-S4 could improve the CMB lower bound on the ULA mass from $\sim 10^{-25}\mathrm{eV}$ to $10^{-23}\mathrm{eV}$, nearing the mass range probed by dwarf galaxy abundances and dark-matter halo density profiles. These improvements will allow for a multi-$\sigma$ detection of percent-level departures from CDM over a wide range of masses. Much of this improvement is driven by the effects of weak gravitational lensing on the CMB, which breaks degeneracies between ULAs and neutrinos. We also find that the addition of ULA parameters does not significantly degrade the sensitivity of the CMB to neutrino masses. These results were obtained using the axionCAMB code (a modification to the CAMB Boltzmann code), presented here for public use.

16 pages, 12 figures. The axionCAMB code will be available online at http://github.com/dgrin1/axionCAMB from 1 August 2016

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• Early Dark Energy Does Not Restore Cosmological Concordance
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• Formation and structure of ultralight bosonic dark matter halos
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• Oscillating Spin-2 Dark Matter
• Dark Sector to Restore Cosmological Concordance
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• Baryon-driven growth of solitonic cores in fuzzy dark matter halos
• Neutrino masses and beyond-$\Lambda$CDM cosmology with LSST and future CMB experiments
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• Fuzzy Dark Matter and the Dark Energy Survey Year 1 Data
• Intensity Mapping as a Probe of Axion Dark Matter
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• Secular effects of Ultralight Dark Matter on Binary Pulsars
• The Spectrum of the Axion Dark Sector
• Dynamical Evidence of a Solitonic Core of $10^9{M}_{\odot }$ in the Milky Way
• Ultra-Light Axion Dark Matter and its impacts on dark halo structure in $N$-body simulation
• Closing the window on fuzzy dark matter with the 21cm signal
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• Cosmology with varying fundamental constants from hyperlight, coupled scalars
• Measuring the Small-Scale Matter Power Spectrum with High-Resolution CMB Lensing
• How sound are our ultra-light axion approximations?
• Axions: From Magnetars and Neutron Star Mergers to Beam Dumps and BECs
• Structure, Kinematics, and Observability of the Large Magellanic Cloud's Dynamical Friction Wake in Cold vs. Fuzzy Dark Matter
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• Improved Mixed Dark Matter Halo Model for Ultralight Axions
• Tests of Neutrino and Dark Radiation Models from Galaxy and CMB surveys
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• Broadband Electrical Action Sensing Techniques with conducting wires for low-mass dark matter axion detection
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• Nonlinear cosmological structure with ultralight bosons via modified gravity
• Hydrodynamics of ultralight complex scalar field dark matter and its impact on the growth of structure
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• Gravitational Wave Resonance in Ultra-Light Dark Matter Halos
• The Effective Field Theory of Large Scale Structure for Mixed Dark Matter Scenarios
• Comparison of two different integration methods for the (1+1)-Dimensional Schrödinger-Poisson Equation
• Constraining Fundamental Constant Variations from Ultralight Dark Matter with Pulsar Timing Arrays
• Emulating the Non-Linear Matter Power-Spectrum in Mixed Axion Dark Matter Models
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• Exploring delaying and heating effects on the 21-cm signature of fuzzy dark matter