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Non-Uniform Cosmological Birefringence and Active Galactic Nuclei · Around

2010

Non-Uniform Cosmological Birefringence and Active Galactic Nuclei

Kamionkowski, Marc

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Cosmological birefringence, a rotation by an angle $\alpha$ of the polarization of photons as they propagate over cosmological distances, is constrained by the cosmic microwave background (CMB) to be $|\alpha|\lesssim1^\circ$ ($1\sigma$) out to redshifts $z\simeq1100$ for a rotation that is uniform across the sky.

However, the rotation angle $\alpha(\theta,\phi)$ may vary as a function of position $(\theta,\phi)$ on the sky.
Here I discuss how a position-dependent rotation can be sought in current and future AGN data.
An upper limit $\VEV{\alpha^2}^{1/2} \lesssim 3.7^\circ$ to the scatter in the position-angle--polarization offsets in a sample of only N=9 AGN already constrains the rotation spherical-harmonic coefficients to $(4\pi)^{-1/2} \alpha_{lm}\lesssim 3.7^\circ$ and constrains the power spectrum for $\alpha$ in models where it is a stochastic field.

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