Curvature Dependence of Peaks in the Cosmic Microwave Background Distribution

Abstract

The widely cited formula ${\ell }_1\simeq 200{\Omega }_0^{-1/2}$ for the multipole number of the first Doppler peak is not even a crude approximation in the case of greatest current interest, in which the cosmic mass density is less than the vacuum energy density. For instance, with ${\Omega }_M$ fixed at 0.3, the position of any Doppler peak varies as ${\Omega }_0^{-1.58}$ near ${\Omega }_0=1$.

7 pages, Latex

References in corpus (2)

• A Flat Universe from High-Resolution Maps of the Cosmic Microwave Background Radiation
• The Cosmic Triangle: Revealing the State of the Universe

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