Python I, II, and III CMB Anisotropy Measurement Constraints on Open and
We use Python I, II, and III cosmic microwave background anisotropy data to constrain cosmogonies. We account for the Python beamwidth and calibration uncertainties. We consider open and spatially-flat-Λ cold dark matter cosmogonies, with nonrelativistic-mass density parameter Ω0 in the range 0.1–1,...
Main Authors: | , , , , , , |
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Other Authors: | |
Format: | Text |
Language: | English |
Published: |
1999
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Subjects: | |
Online Access: | http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.336.5138 http://arxiv.org/pdf/astro-ph/9905127v1.pdf |
Summary: | We use Python I, II, and III cosmic microwave background anisotropy data to constrain cosmogonies. We account for the Python beamwidth and calibration uncertainties. We consider open and spatially-flat-Λ cold dark matter cosmogonies, with nonrelativistic-mass density parameter Ω0 in the range 0.1–1, baryonic-mass density parameter ΩB in the range (0.005–0.029)h −2, and age of the universe t0 in the range (10–20) Gyr. Marginalizing over all parameters but Ω0, the combined Python data favors an open (spatially-flat-Λ) model with Ω0 ≃ 0.2 (0.1). At the 2 σ confidence level model normalizations deduced from the combined Python data are mostly consistent with those drawn from the DMR, UCSB South Pole 1994, ARGO, MAX 4 and 5, White Dish, and SuZIE data sets. Subject headings: cosmic microwave background—cosmology: observations—large-scale structure of the universe 1. |
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