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2010

Polarized CMB Foregrounds: What do we know and how bad is it?

Dickinson, Clive

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Polarized foregrounds are going to be a serious challenge for detecting CMB cosmological B-modes.

Both diffuse Galactic emission and extragalactic sources contribute significantly to the power spectrum on large angular scales.
At low frequencies, Galactic synchrotron emission will dominate with fractional polarization $\sim 20-40%$ at high latitudes while radio sources can contribute significantly even on large ($\sim 1^{\circ}$) angular scales.
Nevertheless, simulations suggest that a detection at the level of $r=0.001$ might be achievable if the foregrounds are not too complex.

Polarized CMB Foregrounds: What do we know and how bad is it? · Around

Built on

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Similar

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2009
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Then

Dunkley, J., et al. 2009, American Institute of Physics Conference Series, 1141, 222
2009
Later among the works it cites.
Hinshaw, G., et al. 2009, ApJS, 180, 225
2009
Later among the works it cites.
Jackson, N., Browne, I. W. A., Battye, R. A., Gabuzda, D., & Taylor, A. C. 2010, MNRAS, 401, 1388
2010
Closest in time.
Macellari, N., Piepaoli, E., Dickinson, C., Vaillancourt, J.. 2010, MNRAS, submitted
2010
Closest in time.

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