2008

How to De-Rotate the Cosmic Microwave Background Polarization

Kamionkowski, Marc

Understand

If the linear polarization of the cosmic microwave background (CMB) is rotated in a frequency-independent manner as it propagates from the surface of last scatter, it may introduce a B-mode polarization.

Here I show that measurement of higher-order TE, EE, EB, and TB correlations induced by this rotation can be used to reconstruct the rotation angle as a function of position on the sky.
This technique can be used to distinguish primordial B modes from those induced by rotation.
The effects of rotation can be distinguished geometrically from similar effects due to cosmic shear.

Built on

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Similar

A. Lue, L. M. Wang and M. Kamionkowski, Phys. Rev. Lett. 83
1999
Cited alongside, same era.
U. Seljak and M. Zaldarriaga, Phys. Rev. Lett. 82
2002
Cited alongside, same era.
W. Hu, M. M. Hedman and M. Zaldarriaga, Phys. Rev. D 67
2003
Cited alongside, same era.
C. M. Hirata and U. Seljak, Phys. Rev. D 67
2003
Cited alongside, same era.
C. Scoccola, D. Harari and S. Mollerach, Phys. Rev. D 70
2004
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Cited in the paper.
A. Hajian and T. Souradeep, arXiv:astro-ph/0501001
Cited in the paper.
V. Gluscevic, A. Cooray, and M. Kamionkowski, in preparation
Original
Cited in the paper.

Then

A. R. Pullen and M. Kamionkowski, Phys. Rev. D 76
Original
2007
Later among the works it cites.
B. Feng et al
Original
2008
Closest in time.
S. Gardner, Phys. Rev. Lett. 100
2008
Closest in time.
K. M. Smith, O. Zahn and O. Dore, Phys. Rev. D 76
Original
2008
Closest in time.

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