WMAP 
SevenYear Wilkinson Microwave Anisotropy Probe (WMAP) Observations:

WMAP Sevenyear Paper Figures, C. Bennett, et al.  
Individual figures are provided for use in talks. Proper display of PNG transparency in PowerPoint requires saving files to your computer before Inserting them. Please acknowledge the WMAP Science Team when using these images. Image Credit: NASA / WMAP Science Team 

Fig.1 (top) A large colder than average region, highlighted by the white curve, appears prominently on the raw Vband temperature map. The full sky map is shown with the Galactic plane horizontal across the center of the map with the Galactic Center at the center of the displayed projection. (bottom) With the foreground signals strongly suppressed by the ILC technique, the highlighted cold spot is seen to be at least as prominent. It is offset from the Galactic Center in both latitude and longitude. This fact, combined with the fact that the clearly effective ILC foreground reduction does not diminish this feature, establishes that this is a CMB fluctuation and not a foreground effect. This feature is not anomalous in that simulated realizations of ΛCDM model skies routinely produce features like this. 
PNG (545 kb 1024x1064 pixels) PNG (2 mb 2048x2129 pixels) EPS (238 kb) 

Fig.2 A visual inspection of the ILC map reveals four elongated valleys of cooler temperature that stretch from about the Galactic equator to nearly the south Galactic pole. Ridges of warmer than average temperature lie between the cooler fingers. These features are a consequence of large scale power in the southern sky. It is more difficult to discern as much large scale power in the northern sky. Cold Spot I is located near the northernmost part of one of the fingers, while Cold Spot II (within the red curve) is near the southernmost part of another finger. 
PNG (367 kb 1024x515 pixels) PNG (1.32 mb 2048x1030 pixels) EPS (171 kb) 

Fig.3 The curve is a BlackwellRao estimate of the relative likelihood of the quadrupole power l(l+1)C_{2}/2π in µK^{2} from WMAP. The WMAP ILC data were smoothed to 5° and the KQ85y7 mask was used, both degraded to res 5. The Gibbs sam pling produced a likelihood that has been marginalized over all other multipoles. The highly nonGaussian likelihood distribution is characteristic of the lowestl multipoles. For l > 32 the curves become nearly Gaussian. The vertical line with the label “ΛCDM” is the expected quadrupole from the full power spectrum ΛCDM model bestfit to the WMAP data. The maximum likelihood of the WMAP measured l = 2 quadrupole is at the vertical dotted line. These two values are consistent to well within the 95% confidence region. The WMAP quadrupole is not anomalously low. 
PNG (22 kb 2048x1454 pixels) PNG (59 kb 4096x2907 pixels) EPS (30 kb) 

Fig.4 The cumulative distribution function of the quadrupoles from the Gibbs sampling based on 300,000 points. The vertical line is the predicted ΛCDM model quadrupole value. The cumulative probability is 0.824 where the vertical line crosses the cumulative distribution function . Since the expected quadrupole from the ΛCDM model is well within the 95% confidence range of the measured quadrupole, accounting for noise and cosmic vari ance, we conclude that the measured quadrupole is not anomalously low. 
PNG (16 kb 2048x1328 pixels) PNG (15 kb 2036x1319 pixels) EPS (21 kb) 

Fig.5 The angular correlation function of the full sky WMAP ILC map is shown (heavy black curve). For comparison, the angular correlation function for the best fit ΛCDM model is also shown (thin black curve), along with the associated 68% and 95% confidence ranges, as determined by Monte Carlo simulations. The angular correlation function of the full sky map is seen to be within the 95% confidence range of the best fit ΛCDM model. This angular correlation function was computed from the C_{l} power spectrum, but is nearly indistinguishable from a pixel pair computation. Either way, there is no evidence of a lack of largescale power. 
PNG (22 kb 2048x1618 pixels) PNG (55 kb 4096x3235 pixels) EPS (23 kb) 

Fig.6 (a) The Χ^{2} per degree of freedom of the 7 year temperaturetemperature power spectrum data relative to the best fit ΛCDM model. Light gray points are from 50 simulations that used the same ΛCDM model with the appropriate noise and cosmic variance included, where the error bars are driven by the number of simulations. The data and simulations were run through the same data analysis pipeline. These simulations were used to help fit the effective fraction of the sky, fsky to use for the data analysis. (b) The Χ^{2} per degree of freedom is compared for the 3year, 5year, and 7year maps. Small differences in the fit model have a negligible effect on these plots. The Χ^{2} per degree of freedom for l ≈ 300 has been slightly growing with additional data, while other multipole moment ranges are more random with additional data. (c) The Χ^{2} per degree of freedom had the same WMAP data been taken in a reverse time order. The l < 400 region appears robust, while the Χ^{2} variations for l > 400 appear more random. (d) Variation of Χ^{2} with the choice of Galactic foreground mask appears random for l > 400. 
PNG (33 kb 1015x2048 pixels) PNG (76 kb 2031x4096 pixels) EPS (88 kb) 

Fig.7 The black curve is the cumulative probability of the WMAP temperature data based on 499 simulations. All of the simulations were drawn from the same ΛCDM model, but Χ^{2} was evaluated with respect to the bestfit model for each realization. Of these, 412 (82.6%) had a lower Χ^{2} than the vertical line at 1224.6. Thus, the WMAP power spectrum is statistically compatible with the model. The red curve is a Χ^{2} distribution with 1170 degrees of freedom, shown for comparison. 
PNG (20 kb 248x1379 pixels) PNG (49 kb 4096x2758 pixels) EPS (31 kb) 

Fig.8 We compute Δl = l  l' correlation properties of C_{l} for nearby multipoles for the WMAP data (blue) and comparable simulations (red). For the most part the data and simulations are in good agreement. The most discrepant correlations in C_{l} are for Δl = 1 near l ~ 320 and Δl ~ 2 near l ~ 280. 
PNG (44 kb 2046x1357 pixels) PNG (107 kb 4096x2717 pixels) EPS (196 kb) 

Fig.9 Top: Even excess E_{l} in the observed power spectrum, in bins of Δl = 50, compared to the mean and scatter from 11436 Monte Carlo realizations. Bottom: E_{l} as in the top plot, converted to significance units by normalizing to the Monte Carlo scatter in each bin. Only the l = 250  299 and l = 300  349 bins show a significance greater than 1σ. 
PNG (25 kb 2048x1968 pixels) PNG (66 kb 4096x3936 pixels) EPS (77 kb) 

Fig.10 Even excess E_{l} in the observed power spectrum, in the l range 250  349, compared to a histogram of the same value as computed from 11436 Monte Carlo realizations. The probability for a random realization to exceed the observed value (PTE) is 0.26%, interpolated directly from the Monte Carlo cumulative distribution. A Gaussian with the same area and standard deviation as the histogram is overplotted, with ±1σ indications. 
PNG (29 kb 2046x1474 pixels) PNG (76 kb 4096x2951 pixels) EPS (73 kb) 

Fig.11 Top: Histogram of max (E_{l}/σ(E_{l})) for each Monte Carlo realization. The maximum is taken over 11 bins of Δl = 50, for l = 50  599. The red vertical line is the observed value of 2.65, with a probability to exceed of 5.11%. Middle: Histogram of max(E_{l}/σ(E_{l})), which is the greatest significance found in any l bin having an odd excess. Although the histograms are not normal distributions, the observed maximum even excess is equivalent to a ~ 1.6σ result, and the observed maximum odd excess of 0.34 at the vertical red line is equivalent to a ~ 2.5σ result. Bottom: The histogram is the same as the one above, but restricted to a preselection of the simulations where the maximum of the significance of the even excess is greater than or equal to the observed even excess. 
PNG (23 kb 1527x2048 pixels) PNG (57 kb 3054x4096 pixels) EPS (52 kb) 

Fig.12 The probability of a greater quadrupoleoctupole alignment is given as a function of the alignment angle, in degrees. The probability given here does not account for the a posteriori selection of a multipole alignment search, nor does it take into account the choice of the quadrupole and the octupole moments in particular. 
PNG (15 kb 2048x1420 pixels) PNG (45 kb 4096x2839 pixels) EPS (19 kb) 

Fig.13 We smooth and square the ILC map, as described in the text, to make a map of (ΔT)^{2} to roughly visualize the anisotropy power in a sky map (A). Cold Spot I is the highest power region at this level of resolution, but several other regions also contribute substantial power at this scale. For map (A), the quadrupole and octupole are aligned to within ~ 1°. To evaluate what regions contribute to this alignment, we mask selected gray areas as shown in the sky maps (B) through (J). Each map is labeled by the degree of quadrupoleoctupole alignment remaining after the gray mask is applied. Masking Cold Spot I in (B) or (H) eliminates any significant alignment. However, keeping those regions and masking other regions, also breaks the alignment to a significant degree. We conclude that no single region or pair of regions generates the alignment. Rather the combination of power from a substantial fraction of the full sky map combine to cause the high degree of quadrupoleoctupole alignment. Note that the chance alignment of CMB power with the Galactic cut region discussed in §5 is apparent in map (A). 
PNG (226 kb 1024x712 pixels) PNG (747 kb 2048x1424 pixels) EPS (389 kb) 

Fig.14 The l = 2 quadrupole map and l = 3 octupole map are added. The combined map is then shown superposed on the ILC map from Figure 2. Note that the quadrupole and octupole components arrange themselves to match the cool fingers and the warm regions in between. The fingers and the alignment of the l = 2 and l = 3 multipoles are intimately connected. 
PNG (604 kb 1020x569 pixels) PNG (2 mb 2036x1134 pixels) EPS (179 kb) 

Fig.15 The probability for a Monte Carlo simulation to have a larger dipole modulation than the coadded V+W WMAP data, as measured by the statistic κ1, is shown as a function of the maximum multipole moment l_{mod} that is assumed to be modulated. This can be interpreted as the statistical significance of power asymmetry for a fixed value of l_{mod}, if one does not account for possible a posteriori bias when chosing lmod. 
PNG (43 kb 2048x1607 pixels) PNG (81 kb 4096x3215 pixels) EPS (27 kb) 

Fig.16 The quadrupolar bipolar power spectra, binned with Δl = 50, is shown separately for Vband and Wband WMAP data, using the KQ75y7 mask. Only the components of the bipolar power spectra that point along the ecliptic axis are shown (i.e. components with M = 0 in ecliptic coordinates). A statistically significant quadrupolar effect is seen, even for a single frequency band in a single angular bin. 
PNG (32 kb 2048x1526 pixels) PNG (77 kb 4096x3052 pixels) EPS (76 kb) 

Fig.17 The “SH” initials of Stephen Hawking are shown in the ILC sky map. The “S” and “H” are in roughly the same font size and style, and both letters are aligned neatly along a line of fixed Galactic latitude. A calculation would show that the probability of this particular occurrence is vanishingly small. Yet, there is no case to made for a nonstandard cosmology despite this extraordinarily low probability event. It is clear that the combined selection of looking for initials, these particular initials, and their alignment and location are all a posteriori choices. For a rich data set, as is the case with WMAP , there are a lot of data and a lot of ways of analyzing the data. Low probability events are guaranteed to occur. The a posteriori assignment of a likelihood for a particular event detected, especially when the detection of that event is “optimized” for maximum effect by analysis choices, does not result in a fair unbiased assessment. This is a recurrent issue with CMB data analysis, and is often a tricky issue and one that is difficult to overcome. 
PNG (314 kb 1024x525 pixels) PNG (1 mb 2048x1050 pixels) EPS (230 kb) 