Interferometric Observations of the Cosmic Microwave Background Radiation

Details Interferometric Observations of the Cosmic Microwave Background Radiation Interferometric Observations of the Cosmic Microwave Background Radiation

2003-06-19

arxiv.org/abs/astro-ph/0306383v1

Astronomy and Astrophysics

Astrophysics

To appear in Carnegie Observatories Astrophysics Series, Vol. 2: Measuring and Modeling the Universe, ed. W. L. Freedman (Camb

Scientific paper

Radio interferometers are well suited to studies of both total intensity and polarized intensity fluctuations of the cosmic microwave background radiation, and they have been used successfully in measurements of both the primary and secondary anisotropy. Recent observations with the Cosmic Background Imager operating in the Chilean Andes, the Degree Angular Scale Interferometer operating at the South Pole, and the Very Small Array operating in Tenerife have probed the primary anisotropy over a wide range of angular scales. The advantages of interferometers for microwave background observations of both total intensity and polarized radiation are discussed, and the cosmological results from these three instruments are presented. The results show that, subject to a reasonable value for the Hubble constant, which is degenerate with the geometry in closed models, the geometry of the Universe is flat to high precision (~5%) and the primordial fluctuation spectrum is very close to the scale-invariant Harrison-Zel'dovich spectrum. Both of these findings are concordant with inflationary predictions. The results also show that the baryonic matter content is consistent with that found from primordial nucleosynthesis, while the cold dark matter component can account for no more than ~40% of the energy density of the Universe. It is a requirement of these observations, therefore, that ~60% of the energy content of the Universe is not related to matter, either baryonic or nonbaryonic. This dark energy component of the energy density is attributed to a nonzero cosmological constant.

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