Abstract
Abstract We develop a strategy to determine the cosmic birefringence and miscalibrated polarization angles simultaneously using the observed $EB$ polarization power spectra of the cosmic microwave background and the Galactic foreground emission. We extend the methodology of Y. Minami et al. (Prog. Theor. Exp. Phys. 2019, 083E02, 2019), which was developed for auto-frequency power spectra, by including cross-frequency spectra. By fitting one global birefringence angle and independent miscalibration angles at different frequency bands, we determine both angles with significantly smaller uncertainties (by more than a factor of two) compared to the auto spectra.
Highlights
Measuring the rotation of polarization directions of photons is a way to search for parity violating physics
We find that the uncertainty in β from the cross frequency power spectra is more than a factor of two smaller than 11 arcmin obtained from the auto frequency spectra [9]
We have developed a strategy to determine the cosmic birefringence (β) and miscalibrated polarization angles (α) of cosmic microwave background (CMB) experiments using the observed EB power spectra of the CMB and Galactic foreground emission
Summary
Measuring the rotation of polarization directions of photons is a way to search for parity violating physics. [9], we lifted the degeneracy by the polarized Galactic foreground emission The miscalibration rotates both CMB and foregrounds by an angle α, whereas the cosmic birefringence rotates only CMB by an angle β; we can use the different multipole dependence of the CMB and the Galactic foreground polarization power spectra to determine α and β simultaneously. [9], which was limited to the auto frequency power spectra, to include the cross frequency spectra. [9], we showed that an experiment similar to LiteBIRD [10] can determine β with a precision of 11 arcmin using the auto frequency power spectra, simultaneously with α.1. In this paper we show that we can reduce the uncertainty by more than a factor of two by including the cross frequency spectra.
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