In every direction, there is a very low energy and very uniform
radiation that we see
filling the Universe. This is called the 3 Degree
Kelvin Background Radiation, or the Cosmic Background Radiation, or
the Microwave Background. These names come about because this radiation
is essentially a black body with temperature slightly less than 3 degrees Kelvin
(about 2.76 K), which peaks in the microwave portion of the spectrum.
This radiation is the strongest evidence for the validity of the
hot big bang model.
The adjacent figure shows the essentially perfect blackbody spectrum obtained by
Explorer (COBE) satellite.
The following image was taken by
shows the temperature of the cosmic background radiation plotted in galactic
coordinates, with red cooler and blue and violet hotter
(Ref). This dipole anisotropy
is because of the Doppler effect. If the Earth moves with respect to the microwave background,
it will be blue shifted to a higher effective temperature in the direction of the Earth's motion and red
shifted to a lower effective temperature in the direction opposite the Earth's motion.
The indication of the above image is that the local group of galaxies, to which the Earth belongs,
is moving at about 600 km/s with respect to the background radiation. It is not know why the Earth is
moving with such a high velocity relative to the background radiation.
Evidence for the Big Bang
The cosmic background radiation (sometimes called the CBR),
is the afterglow of the big bang, cooled to a faint
whisper in the microwave spectrum
by the expansion of the Universe for 15 billion years (which causes the radiation
originally produced in the big bang to redshift to longer wavelengths).
As shown in the
map of the background radiation
in different directions
taken by the Differential Microwave Radiometer on NASA's
is not completely uniform, though it is very nearly so
(Ref). To obtain this image, the average dipole
anisotropy exhibited in the image above has been subtracted out, since it represents a Doppler shift due to
the Earth's motion. Thus, what remains should represent true variations in the temperature of the
In this image,
red denotes hotter fluctuations and blue and black denote cooler
fluctuations around the average. These fluctuations are extremely small,
representing deviations from the average of only about 1/100,000
of the average temperature of the observed background radiation.
Problems with the Uniformity
isotropic nature of the
cosmic background radiation
indicates that the early stages of the Universe were almost
completely uniform. This raises two problems for the big bang theory.
First, when we look at the microwave background coming from widely separated parts
of the sky it can be shown that these regions are too separated to have been able
to communicate with each other even with signals travelling at light velocity.
Thus, how did they know to have almost exactly the same temperature? This general
problem is called the horizon problem.
the present Universe is homogenous and isotropic, but only on very large scales.
For scales the size of superclusters and smaller
matter in the universe
is quite lumpy, as illustrated in the following
FIGURE: Data from the survey of galaxies.
The voids and
"walls" that form the large-scale structure are mapped here by 11,000 galaxies.
Our galaxy, the Milky Way,
is at the center. The outer radius is at a distance of
approximately 450 million light-years.
Obscuration by the plane of the Milky Way is responsible for the missing
pie-shaped sectors to the right and left. Click on the image to get a larger
(Smithsonian Astrophysical Observatory, 1993. Northern
data (top)--Margaret Geller and John
Huchra, Southern data (bottom)--Luiz da Costa et al. Quoted in
Cosmology, a Research
Briefing, National Academy of Sciences.)
Thus, the discovery of small deviations from smoothness (anisotopies) in
the cosmic microwave background is welcome, for it provides at least
the possibility for the seeds around which structure formed in the later Universe.
However, as we shall see, we are still far from a quantitative understanding of how
this came to be.