Center for Astrophysical Research in Antarctica
T/T 
10
) in the
angular distribution of
microwave power. The amplitude and spatial distribution of the
anisotropy are directly related to the conditions in the early Universe
which gave rise to the onset of structure formation. All current models
of structure formation predict specific power spectra and morphologies
for the CMB anisotropy. Within the context of a given theory, the
cosmological parameters such as the Hubble constant H
, and
the mass density of the Universe 
= 
/
, can be
estimated from observations of the anisotropy in the CMB. Determining
the angular power spectrum of the fluctuations, their distribution
function, and imaging the CMB anisotropy at intermediate angular
scales (20 arcseconds to 1 degree)
is the scientific goal of the CARA CMB program. Measuring the angular power spectrum of the CMB fluctuations, and producing images of the primary and secondary anisotropy of the CMB, are key science goals of CARA experiments. Each experiment addresses a unique range of angular scales and frequency coverage. Together, they span a range of angular scales from 3 degrees to 2 arcminutes, and frequencies from 26 - 400 GHz.
CARA CMB instruments include:
Questions? Comments? email us at caraweb@astro.uchicago.edu Last modified Monday, 06-Dec-1999 08:43:47 CST