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- W4282840334 abstract "A pseudoscalar axionlike field, $phi$, may explain the $3sigma$ hint of cosmic birefringence observed in the $EB$ power spectrum of the cosmic microwave background (CMB) polarization data. Is $phi$ dark energy or dark matter? A tomographic approach can answer this question. The effective mass of dark energy field responsible for the accelerated expansion of the Universe today must be smaller than $m_phisimeq 10^{-33}$ eV. If $m_phi gtrsim 10^{-32}$ eV, $phi$ starts evolving before the epoch of reionization and we should observe different amounts of birefringence from the $EB$ power spectrum at low ($llesssim 10$) and high multipoles. Such an observation, which requires a full-sky satellite mission, would rule out $phi$ being dark energy. If $m_phi gtrsim 10^{-28}$ eV, $phi$ starts oscillating during the epoch of recombination, leaving a distinct signature in the $EB$ power spectrum at high multipoles, which can be measured precisely by ground-based CMB observations. Our tomographic approach relies on the shape of the $EB$ power spectrum and is less sensitive to miscalibration of polarization angles." @default.
- W4282840334 created "2022-06-15" @default.
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- W4282840334 date "2022-06-14" @default.
- W4282840334 modified "2023-10-17" @default.
- W4282840334 title "Is cosmic birefringence due to dark energy or dark matter? A tomographic approach" @default.
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- W4282840334 doi "https://doi.org/10.1103/physrevd.105.123509" @default.
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