1994/02/24 by David N. Spergel, Spergel, David N., Ue‐Li Pen +6
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics (astro-ph) #Cosmology and Gravitation Theories #FOS: Physical sciences #Geophysics and Gravity Measurements #High Energy Physics - Phenomenology (hep-ph) #Radio Astronomy Observations and Technology #astro-ph #hep-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9402060
ten pages and 6 included figures, LaTeX with epsf for figures
arxiv created 1994/02/24 · openalex publication_date 1994/02/24 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
( to appear in: Proceedings of the Nishonomiya Yukawa Memorial Symposium Edited by M. Sasaki) There are several models for generating fluctuations in an open universe that are compatible with the microwave background fluctuations detected by COBE \it and observations of large scale structure. Topological defects, such as strings and textures, appear to be more successful in a low-Ω model than in an Ω= 1 model. These models predict that the cosmic microwave background (CMB) fluctuations are non-Gaussian with distinctive signatures that may lead to their confirmation. If there exists a mechanism for generating scale invariant mass fluctuations, (δM/M)2 ∝ M-4/3, then these models are also compatible with COBE. Both models predict mass fluctuations on the 8/h Mpc scale, σ8, ∼ 0.5 - 1 for Ωh ∼ 0.2 - 0.3. A variety of observations of large-scale structure, clusters and galaxies, as well as the age problem, suggest that the low-Ω models are attractive.