Curvature Dependence of Peaks in the Cosmic Microwave Background Distribution

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dc.creatorWeinberg, Steven
dc.date2000-06-20
dc.date.accessioned2026-07-07T11:28:41Z
dc.date.available2026-07-07T11:28:41Z
dc.descriptionThe widely cited formula $\ell_1\simeq 200 Ω_0^{-1/2}$ 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 $Ω_M$ fixed at 0.3, the position of any Doppler peak varies as $Ω_0^{-1.58}$ near $Ω_0=1$.
dc.description7 pages, Latex
dc.identifierhttps://arxiv.org/abs/astro-ph/0006276
dc.identifierhttp://arxiv.org/abs/astro-ph/0006276
dc.identifierPhys.Rev.D62:127302,2000
dc.identifierdoi:10.1103/PhysRevD.62.127302
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/196472
dc.subjectAstrophysics
dc.titleCurvature Dependence of Peaks in the Cosmic Microwave Background Distribution
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