Curvature Dependence of Peaks in the Cosmic Microwave Background Distribution

Details Curvature Dependence of Peaks in the Cosmic Microwave Background Distribution Curvature Dependence of Peaks in the Cosmic Microwave Background Distribution

2000-06-20

arxiv.org/abs/astro-ph/0006276v1

Phys.Rev.D62:127302,2000

Astronomy and Astrophysics

Astrophysics

7 pages, Latex

Scientific paper

10.1103/PhysRevD.62.127302

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 $\Omega_0=1$.

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