Polarization Analysis

Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Polarization Analysis, L. Page, et al., 2007ApJS..170..335P, reprint / preprint (2.2MB) / bundled figures (10.6MB) / individual figures / ADS / astro-ph

WMAP Three-year Paper Figures, Page et al.
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	Fig. 1 A model of the ionization history of the universe. The line marked "x" is the ionization fraction, x=ne/n where ne is the number of electrons and n=11.2ωb(1+z)3 m-3 is the number of protons with ωb the baryon density.	PNG (45 kb - 452x512 pixels) PNG (57 kb - 903x1024 pixels) EPS (14 kb)
	Fig. 2 Top: Map of Tau A in Galactic coordinates at 41 GHz in Stokes I, Q, U, P, smoothed to 1o. Since Tau A is polarized parallel to the Galactic plane it is negative in Q and small in U. Bottom: Map of Centaurus A in Stokes I, Q, U, and P.	PNG (119 kb - 454x512 pixels) PNG (329 kb - 908x1024 pixels) EPS (592 kb)
	Fig. 3 P and γ maps for K, Ka, and Q bands in Galactic coordinates. There is only one polarization map for K and Ka bands. For Q band, there are two maps which have been coadded. The maps are smoothed to 2o.	PNG (900 kb - 512x843 pixels) PNG (3.0 mb - 1024x1685 pixels) EPS (766 kb)
	Fig. 4 Similar to Figure 3 but for V and W bands. The two V-band maps have been coadded as have the four W-band maps. The relatively higher noise in the ecliptic plane is evident. Maps of the noise bias have been subtracted in these images.	PNG (454 kb - 512x573 pixels) PNG (1.8 mb - 1024x1145 pixels) EPS (473 kb)
	Fig. 5 A Lambert azimuthal equal area projection of the Galactic poles (left: north) showing the K-band polarization. The circumference of each map is at zero Galactic latitude.	PNG (272 kb - 297x512 pixels) PNG (966 kb - 594x1024 pixels) EPS (513 kb)
	Fig. 6 Stokes Q and U maps in 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.	PNG (414 kb - 447x650 pixels) PNG (2.1 mb - 894x1300 pixels) EPS (649 kb)
	Fig. 7 Left: The angle of the magnetic field, γM=γPA+90o, derived from the synchrotron radiation in the K-band map. Right: The predicted magnetic field direction given by a simple model of the electron distribution and the logarithmic spiral arm model.	PNG (197 kb - 208x650 pixels) PNG (658 kb - 415x1300 pixels) EPS (675 kb)
	Fig. 8 The left panel shows the geometric suppression factor, gsync, in the polarization due to the magnetic field geometry. The right panel shows a similar geometric suppression factor for polarized dust emission.	PNG (30 kb - 180x508 pixels) PNG (296 kb - 365x1024 pixels) EPS (692 kb)
	Fig. 9 Left: The observed K-band polarization, P. The color scale ranges from 0 to 0.1 mK. Right: The model prediction of the K-band polarization based on the Haslam intensity map.	PNG (198 kb - 240x650 pixels) PNG (709 kb - 480x1300 pixels) EPS (1.3 mb)
	Fig. 10 Top: The Haslam 408 MHz map is shown with circles indicating loops from Berkhuijsen et al. (1971). Bottom: The WMAP K-band polarization map with the same loops superimposed. (1971).	PNG (571 kb - 512x629 pixels) PNG (2.3 mb - 1024x1257 pixels) EPS (747 kb)
	Fig. 11 A map of the correlation, Z, between the polarization angle derived from the polarization of starlight, and the polarization angle in K-band. In the regions of high Kband polarization, the correlation is strong.	PNG (86 kb - 374x512 pixels) PNG (515 kb - 748x1024 pixels) EPS (476 kb)
	Fig. 12 The upper panels show the polarization signal at W band with the CMB and synchrotron signal removed (smoothed with a 10o Gaussian beam). The lower panels show the predicted dust polarization based on Equation 15.	PNG (402 kb - 434x650 pixels) PNG (1.3 mb - 867x1300 pixels) EPS (1.1 mb)
	Fig. 13 Temperature maps of the low polarization components for K, Q, and W bands. The maps are computed using equation (16). The color scale is in mK. Near the Galactic center, the low polarization component is approximately 6%, 3%, and 6% of the unpolarized emission in K, Q, and W bands respectively.	PNG (328 kb - 452x650 pixels) PNG (1.4 mb - 904x1300 pixels) EPS (925 kb)
	Fig. 14 The polarization masks, in Galactic coordinates, are shown for the P02, P04, P06, and P10 cut levels. The cross hatched region along the Galactic plane, common to all polarization masks, shows the dust intensity cut.	PNG (181 kb - 348x650 pixels) PNG (339 kb - 695x1300 pixels) EPS (505 kb)
	Fig. 15 The Ka, Q, V, and W band Q Stokes Parameter maps before and after foreground subtraction using the method outlined in §4.3. There is a possible residual signal in W band though the noise is not yet sufficiently low to be certain.	PNG (375 kb - 432x512 pixels) PNG (1.1 mb - 863x1024 pixels) EPS (671 kb)
	Fig. 16 A comparison of the predicted Cl errors with (black) and without (red) assuming correlated noise in the polarization sky maps. On the y-axis is plotted the diagonal element of the inverse of the Fisher matrix for one year of data.	PNG (14 kb - 382x512 pixels) PNG (35 kb - 764x1024 pixels) EPS (67 kb)
	Fig. 17 The absolute value of the EE (solid, violet through green) and BB (dashed, violet through green) polarization spectra for the region outside the P06 mask. The best fit ΛCDM model to TT, TE, and EE data with τ=0.09 and an additional tensor contribution with Γ=0.3 is shown in black.	PNG (16 kb - 484x512 pixels) PNG (37 kb - 968x1024 pixels) EPS (16 kb)
	Fig. 18 The frequency spectrum of the EE and BB power spectra for the region outside the P06 mask. To increase the signal to noise ratio, multiple values of l are averaged as indicated. Only statistical errors are shown. Negative values are not plotted.	PNG (15 kb - 392x512 pixels) PNG (38 kb - 784x1024 pixels) EPS (26 kb)
	Fig. 19 The frequency spectrum of the foreground cleaned EE and BB power spectra outside the P06 mask for l=2-9. Black shows EE, blue shows BB, and green, cyan, and orange show the EE yi-yj spectra (the BB ones are similar).	PNG (18 kb - 363x750 pixels) PNG (43 kb - 726x1500 pixels) EPS (71 kb)
	Fig. 20 The TB, EB, BB spectra for the region outside the P06 mask. These spectra are expected to be null. For T, the foreground-cleaned V and W bands have been combined. For E and B, the foreground-cleaned Q and V bands have been combined.	PNG (10 kb - 512x512 pixels) PNG (22 kb - 1024x1024 pixels) EPS (21 kb)
	Fig. 21 Top: The EE and BB power spectra outside the P06 mask before and after applying the KD3Pol foreground model. Bottom: Expanded plots of the QV data for the P06 cut.	PNG (21 kb - 462x512 pixels) PNG (57 kb - 924x1024 pixels) EPS (36 kb)
	Fig. 22 The EE spectrum at l > 40 for all measurements of the CMB polarization. The curve is the best fit EE spectrum. Note that the y axis has only one power of l. The black boxes are the WMAP data; the triangles are the BOOMERanG data; the squares are the DASI data; the diamonds are the CBI data; and the asterisk is the CAPMAP data.	PNG (12 kb - 466x512 pixels) PNG (27 kb - 931x1024 pixels) EPS (141 kb)
	Fig. 23 Left: Lines of Δ&Chi2 for the fit given in Equation 28 vs. AEE. The different colors correspond to different frequency combinations. Right: The amplitude and phase of the TE measurement with respect to the model predicted by the TT data.	PNG (10 kb - 236x512 pixels) PNG (25 kb - 472x1024 pixels) EPS (21 kb)
	Fig. 24 The TE power spectra for high and low l ranges for the region outside the P06 mask in EE and TT.	PNG (13 kb - 237x512 pixels) PNG (37 kb - 474x1024 pixels) EPS (19 kb)
	Fig. 25 Plots of signal for TT (black), TE (red), EE (green) for the best fit model. The dashed line for TE indicates areas of anticorrelation. The cosmic variance is shown as a light swath around each model.	PNG (14 kb - 477x512 pixels) PNG (33 kb - 953x1024 pixels) EPS (65 kb)
	Fig. 26 The relative likelihoods of τ from the stand alone exact likelihood code and the first-year analysis. For the three-year results, all parameters except τ and the scalar normalization, A, were held fixed as described in the text.	PNG (15 kb - 446x512 pixels) PNG (38 kb - 892x1024 pixels) EPS (14 kb)
	Fig. 27 The two dimensional likelihood as a function of Τ and Γ for the BB spectrum. The contours indicate 1σ and 2σ. The ns parameter, which is degenerate with Τ and Γ, has been set at ns = 0.96.	PNG (10 kb - 512x512 pixels) PNG (23 kb - 1024x1024 pixels) EPS (42 kb)
	Fig. 28 The correlation coefficients of the Fisher matrices. The diamonds are derived from 100,000 Monte Carlo simulations, while the solid lines are the analytical formulae in the noise-dominated regime.	PNG (19 kb - 501x512 pixels) PNG (46 kb - 1024x1024 pixels) EPS (42 kb)