Fig. 8 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. 8.

Left: Geometric suppression factor, ﹩g_{\mathrm{sync}\,}( \hat{n}) ﹩, in the polarization due to the magnetic field geometry. In the region of low polarization, ﹩g_{\mathrm{sync}\,}( \hat{n}) ﹩ is bounded to be greater than 0.2. Right: Similar geometric suppression factor for polarized dust emission, ﹩g_{\mathrm{dust}\,}( \hat{n}) ﹩; see § 4.1.3.

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