1997/11/12 by J. Lesgourgues, David Polarski, D. Polarski +2 · 3 citations
Physics and Astronomy · #Astrophysics #Black Holes and Theoretical Physics #Cold dark matter #Cosmic background radiation #Cosmic microwave background #Cosmological constant #Cosmology and Gravitation Theories #Dark matter #Fundamental plane (elliptical galaxies) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Inflation (cosmology) #Inflaton #Physics #Quantum mechanics #Spectral density #Theoretical physics #astro-ph #gr-qc #hep-ph
paper · pdf · doi:10.1046/j.1365-8711.1998.01537.x
published as Mon.Not.Roy.Astron.Soc. 297 (1998) 769-776 · 7 pages, 5 figures, LaTeX with mn.sty
arxiv created 1997/11/12 · openalex publication_date 1998/07/01 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
A class of spatially flat models with cold dark matter (CDM), a cosmological constant and a broken-scale-invariant (BSI) step-like primordial (initial) spectrum of adiabatic perturbations, generated in an exactly solvable inflationary model where the inflaton potential has a rapid change of its first derivative at some point, is confronted with existing observational data on angular fluctuations of the CMB temperature, galaxy clustering and peculiar velocities of galaxies. If we locate the step in the initial spectrum at k ≃ 0.05 h Mpc−1, where a feature in the spectrum of Abell clusters of galaxies was found that could reflect a property of the initial spectrum, and if the large-scale flat plateau of the spectrum is normalized according to the COBE data, the only remaining parameter of the spectrum is p— the ratio of amplitudes of the metric perturbations between the small-scale and large-scale flat plateaux. Allowed regions in the plane of parameters (Ω = 1 − ΩΛ, H0) satisfying all data have been found for p lying in the region (0.8–1.7). Especially good agreement of the form of the present power spectrum in this model with the form of the cluster power spectrum is obtained for the inverted step (p < 1, p = 0.7–0.8), when the initial spectrum has slightly more power on small scales.