Pseudoscalar perturbations and polarization of the cosmic microwave background

Details Pseudoscalar perturbations and polarization of the cosmic microwave background Pseudoscalar perturbations and polarization of the cosmic microwave background

2008-08-05

arxiv.org/abs/0808.0673v1

Phys.Rev.Lett.103:051302,2009

Astronomy and Astrophysics

Astrophysics

4 pages, 1 figure

Scientific paper

10.1103/PhysRevLett.103.051302

We show that models of new particle physics containing massless pseudoscalar fields super-weakly coupled to photons can be very efficiently probed with CMB polarization anisotropies. The stochastic pseudoscalar fluctuations generated during inflation provide a mechanism for converting E-mode polarization to B-mode during photon propagation from the surface of last scattering. The efficiency of this conversion process is controlled by the dimensionless ratio H/(2\pi f_a), where H is the Hubble scale during inflation, and f_a^{-1} is the strength of the pseudoscalar coupling to photons. The current observational limits on the B-mode constrain this ratio to be less than 0.07, which in many models of inflation translates to a sensitivity to values of f_a in excess of 10^{14} GeV, surpassing the sensitivity of other tests.

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