2005/12/13 by Shiro Hirai, Tomoyuki Takami · 10 citations
Physics and Astronomy · #Anisotropy #Black Holes and Theoretical Physics #CMB cold spot #Cosmic background radiation #Cosmic microwave background #Cosmology and Gravitation Theories #Galaxies: Formation, Evolution, Phenomena #Inflation (cosmology) #Scalar (mathematics) #Spectral density #Spectral line #astro-ph
paper · pdf · doi:10.1088/0264-9381/23/7/019
published in Classical and Quantum Gravity 23(7), 2541-2558 (IOP Publishing) · 41 pages, 11 figures
arxiv created 2005/12/13 · openalex publication_date 2006/03/17 · arxiv updated 2015/06/24 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The effect of the length of inflation on the power spectra of scalar and tensor perturbations is estimated using the power-law inflation model with a scale factor of a (η) = (−η) p = t q . Considering various pre-inflation models with radiation-dominated or scalar matter-dominated periods before inflation in combination with two matching conditions, the temperature angular power spectrum (TT) and temperature–polarization cross-power spectrum (TE) are calculated and a likelihood analysis is performed. It is shown that the discrepancies between the Wilkinson microwave anisotropy probe (WMAP) data and the ΛCDM model, such as suppression of the spectrum at l = 2, 3 and oscillatory behaviour, may be explained by the finite length of inflation model if the length of inflation is near 60 e -folds and q ⩾ 300. The proposed models retain similar values of χ 2 to that achieved by the ΛCDM model with respect to fit to the WMAP data, but display different characteristics of the angular TE power spectra at l ⩽ 20.