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WMAP 3-Year Paper Figures
| WMAP 3-year Paper Figures, Kogut et al. | ||
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Figures from the paper "Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Foreground Polarization" in a form suitable for use in talks. Please acknowledge the WMAP Science Team when using these images. |
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Fig. 1 Estimated signal variance at each WMAP frequency band for 3.°7 pixels. The solid line shows a two-component fit with power-law synchrotron and thermal dust emission assuming no spatial correlations between the two components. |
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Fig. 2 Spectral index of polarized synchrotron emission between 22 and 33 GHz (Mollweide projection in Galactic coordinates). The map has been smoothed with a position-dependent tophat varying from 7° radius near the plane to 18° radius at high latitude. |
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Fig. 3 Spectral index of polarized synchrotron emission binned by Galactic latitude. The spectral index steepens off the Galactic plane. Similar behavior is observed in external edge-on spiral galaxies. |
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Fig. 4 Polarized synchrotron model parameters. (Top) Antenna temperature P = (Q²+U²)0.5 of polarized synchrotron emission at K band. Vectors indicate the polarization direction. (Bottom) Synchrotron fractional polarization, derived by dividing the polarized model by the unpolarized maximum-entropy synchrotron model at K band. |
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Fig. 5 Histogram of synchrotron fractional polarization fs. (Top) High latitude region outside the P06 mask. (Middle) Mid-latitude region inside P06 but with |b| > 5°. (Bottom) Galactic plane, |b| < 5°. |
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Fig. 6 Synchrotron fractional polarization fs binned by Galactic latitude for the northern (filled symbols) and southern (open symbols) hemispheres. Each point shows the mean fractional polarization fs for all pixels in a latitude bin with signal-to-noise ratio greater than one. |
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Fig. 7 Polarized foreground model and residuals for the pixel-by-pixel polarization model. (Left) Antenna temperature of polarized emission at each band. The polarization direction is not shown. (Right) Residuals after subtracting foreground model. |
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Fig. 8 CMB power spectra outside the P06 mask, derived from Q and V band data after subtracting two different foreground models. (top) EE power spectra. (bottom) BB power spectra. The CMB spectra are robust with respect to different foreground models. |
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