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.
The CMB angular power spectrum for WMAP, COBE, ACBAR, and CBI data.
Note that the WMAP results are consistent with the other experiments, and that the
combined WMAP and CBI points constrain the angular power spectrum of our sky
with great accuracy and precision. The WMAP best fit model is also shown.
Please acknowledge the WMAP Science Team when using these images.
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.
Internal Linear Combination Map Linear scale from -200 to 200 uK
The synchrotron, free-free and thermal dust foreground models derived
from WMAP data using the Maximum Entropy Method (MEM) are shown at the frequencies
where each foreground is most dominant.
Please acknowledge the WMAP Science Team when using these images.
Synchrotron map for K band Linear scale from -1 to 5 mK
Three-color maps from the Maximum Entropy Method (MEM) model
for the 5 WMAP frequency bands. These maps indicate which emission mechanism
dominates as a function of frequency and sky position. Synchrotron is red,
free-free is green, and thermal dust is blue.
Please acknowledge the WMAP Science Team when using these images.
A guide to the microwave sky for reference.
This picture shows the large-scale emission from the Milky
Way galaxy, including some of its notable components such
as the Cygnus complex, the North Polar Spur, the Gum region,
etc. The small circles show positions of significant microwave
point sources. The brighter sources are labeled for reference.
Please acknowledge the WMAP Science Team when using these images.
WMAP uses a set of standard sky masks for certain data processing
and analysis needs. The masking is based on the K-band signal
levels, which each successive mask increasing the severity of
the masking cut. The most severe cut is Kp0. Not shown are
additional cuts made around point sources.
Please acknowledge the WMAP Science Team when using these images.
WMAP uses in-flight observations of Jupiter to characterize the beam for each antenna feed.
Window functions are computed from these observations for each of the ten differencing assemblies.
Please acknowledge the WMAP Science Team when using these images.
Side A Focal Plane Mosaic
Each beam response has been normalized to its peak value.
Linear scale from -.5 to 1