Fig. 6 from Three‐Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Polarization Analysis

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Three‐Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Polarization Analysis

Authors: L. Page, G. Hinshaw, E. Komatsu, M. R. Nolta, D. N. Spergel, C. L. Bennett, C. Barnes, R. Bean, O. Doré, J. Dunkley, M. Halpern, R. S. Hill, N. Jarosik, A. Kogut, M. Limon, S. S. Meyer, N. Odegard, H. V. Peiris, G. S. Tucker, L. Verde, J. L. Weiland, E. Wollack, and E. L. Wright

Page et al. 2007 The Astrophysical Journal Supplement Series 170 335.

Provider: AAS Journals

Caption: Fig. 6.

Stokes Q and U maps in the K and Ka bands. The Galactic plane is dominated by positive Stokes Q because the foreground polarization direction is perpendicular to the plane. As discussed in § 4, this is expected because the Galactic magnetic field is predominantly parallel to the plane. For comparison, the Stokes Q and U maps of a noiseless CMB simulation have peak‐to‐peak values of less than 6 μK. These maps have been smoothed to 1°.

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