WMAP Data Product Images

WMAP Seven-year Paper Figures

Figures from the Seven-Year WMAP papers in a form suitable for use in talks.

Please acknowledge the WMAP Science Team when using these images.
Jarosik, et al.
Figures from the paper "Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Data Processing, Sky Maps, and Basic Results" in a form suitable for use in talks. Please acknowledge the WMAP Science Team when using these images.
 (Images)
Gold, et al.
Figures from the paper "Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Data Processing, Galactic Foreground Emission" in a form suitable for use in talks. Please acknowledge the WMAP Science Team when using these images.
 (Images)
Larson, et al.
Figures from the paper "Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Data Processing, Power Spectra and WMAP Derived Parameters" in a form suitable for use in talks. Please acknowledge the WMAP Science Team when using these images.
 (Images)
Bennett, et al.
Figures from the paper "Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Data Processing, Are There Cosmic Microwave Background Anomalies" in a form suitable for use in talks. Please acknowledge the WMAP Science Team when using these images.
 (Images)
Komatsu, et al.
Figures from the paper "Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Data Processing, Cosmological Interpretation" in a form suitable for use in talks. Please acknowledge the WMAP Science Team when using these images.
 (Images)
Weiland, et al.
Figures from the paper "Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Data Processing, Planets and Celestial Calibration Sources" in a form suitable for use in talks. Please acknowledge the WMAP Science Team when using these images.
 (Images)

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WMAP Full-sky Temperature Maps

The images below represent full-sky maps of the cosmic microwave background anisotropy and foreground signal from our galaxy (in red). The 5 frequency maps are constructed from the differential time-ordered observations of the ten WMAP differencing assemblies. Galactic foreground is stongest in K band, weakest in V and W bands.

Please acknowledge the WMAP Science Team when using these images.
K-Band K-Band Map (23 GHz)
Linear scale from -200 to 200 uK
 PNG (62 kb - 256x512 pixels)
PNG (211 kb - 512x1024 pixels)
PNG (715 kb - 1024x2048 pixels)
K-Band Ka-Band Map (33 GHz)
Linear scale from -200 to 200 uK
 PNG (79 kb - 256x512 pixels)
PNG (285 kb - 512x1024 pixels)
PNG (1.2 mb - 1024x2048 pixels)
Q-Band Q-Band Map (41 GHz)
Linear scale from -200 to 200 uK
 PNG (85 kb - 256x512 pixels)
PNG (312 kb - 512x1024 pixels)
PNG (1.1 mb - 1024x2048 pixels)
V-Band V-Band Map (61 GHz)
Linear scale from -200 to 200 uK
 PNG (90 kb - 256x512 pixels)
PNG (334 kb - 512x1024 pixels)
PNG (1.2 mb - 1024x2048 pixels)
W-Band W-Band Map (94 GHz)
Linear scale from -200 to 200 uK
 PNG (89 kb - 256x512 pixels)
PNG (326 kb - 512x1024 pixels)
PNG (1.2 mb - 1024x2048 pixels)

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WMAP CMB Power Spectra

Temperature and polarization power spectra derived from the WMAP Seven-year data. Data are represented as points, curves correspond to the best-fit LCDM model, and shaded regions delineate cosmic variance about the model.

Please acknowledge the WMAP Science Team when using these images.
Power Spectra WMAP Seven-Year TT and TE Power Spectra
See Fig. 9 of Jarosik et al. (2010)
 PNG (36 kb - 2048x2185 pixels)
PNG (85 kb - 4096x4369 pixels)
Power Spectra WMAP Seven-Year TT Power Spectra
See Fig. 1 of Larson et al. (2010)
 PNG (23 kb - 1285x2048 pixels)
PNG (55 kb - 2570x4096 pixels)

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WMAP Internal Linear Combination Map

The Internal Linear Combination Map is a weighted linear combination of the five WMAP frequency maps. The weights are computed using criteria which minimize the Galactic foreground contribution to the sky signal. The resultant map provides a low-contamination image of the CMB anisotropy.

Please acknowledge the WMAP Science Team when using these images.
W-Band Internal Linear Combination Map
Galactic coordinates,
Mollweide projection
Linear scale from -200 to 200 uK
 PNG (88 kb - 256x512 pixels)
PNG (283 kb - 512x1024 pixels)
PNG (893 kb - 1024x2048 pixels)

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WMAP Polarizing Pattern

The standard model predicts a specific linked pattern of temperature and polarization around hot and cold spots in the map. WMAP now sees the predicted pattern in the map, as shown in the figure.

Please acknowledge the WMAP Science Team when using these images.
W-Band WMAP Polarizing Pattern
WMAP has produced a visual demonstration that the polarization pattern around hot and cold spots follows the pattern expected in the standard model.
 JPG (111 kb - 354x640 pixels)
JPG (304 kb - 566x1024 pixels)
PNG (155 kb - 2264x4096 pixels)
ZIP (283 kb)

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Stacked Polarization Cold Spot

Please acknowledge the WMAP Science Team when using these images.
pol Stacked Polarization Cold Spot

 JPG (129 kb - 640x427 pixels)
PNG (272 kb - 1026x685 pixels)
PNG (366 kb - 2052x1370 pixels)
ZIP (674 kb)

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Stokes Q and U Sky Images

Please acknowledge the WMAP Science Team when using these images.
Stokes Stokes Q and U Sky Images
Plots of the seven-year average Stokes Q and U maps in Galactic coordinates. All maps have been smoothed with a 2° FWHM Gaussian kernel.
 PNG (81 kb 512x256 pixels)
PNG (83 kb 512x256 pixels)
PNG (72 kb 512x256 pixels)
PNG (72 kb 512x256 pixels)
PNG (67 kb 512x256 pixels)
PNG (67 kb 512x256 pixels)
PNG (66 kb 512x256 pixels)
PNG (66 kb 512x256 pixels)
PNG (77 kb 512x256 pixels)
PNG (76 kb 512x256 pixels)
PNG (3 kb 506x60 pixels)

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A service of the HEASARC and of the Astrophysics Science Division at NASA/GSFC
Goddard Space Flight Center, National Aeronautics and Space Administration
HEASARC Director: Dr. Alan P. Smale
LAMBDA Director: Dr. David T. Chuss
NASA Official: Dr. David T. Chuss
Web Curator: Michael R. Greason