2002/05/23 by J. L. Sievers, Jonathan Sievers, J. Richard Bond +19 · 1 voice · 218 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Baryon #COSMIC cancer database #Cosmic background radiation #Cosmic microwave background #Cosmic variance #Cosmology #Cosmology and Gravitation Theories #Decoupling (probability) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Maxima #Physics #Quantum mechanics #Redshift #Reionization #Spectral density #Spectral index #Spectral line #Statistics #astro-ph
paper · pdf · doi:10.1086/375510
published in The Astrophysical Journal 591(2), 599-622 (IOP Publishing) · Accepted by the Astrophysical Journal; 22 pages including 14 color figures. v2: new analysis with better sampling in parameter space and including VSA data
arxiv created 2003/03/11 · openalex publication_date 2003/07/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We report on the cosmological parameters derived from observations with the Cosmic Background Imager (CBI), covering 40 deg 2 and the multipole range 300 ≲ l ≲ 3500. The angular scales probed by the CBI correspond to structures that cover the mass range from 10 14 to 10 17 M ☉ , and the observations reveal, for the first time, the seeds that gave rise to clusters of galaxies. These unique, high-resolution observations also show damping in the power spectrum to l ~ 2000, which we interpret as being due to the finite width of the photon-baryon decoupling region and the viscosity operating at decoupling. Because the observations extend to much higher l , the CBI results provide information complementary to that probed by the BOOMERANG, DASI, MAXIMA, and VSA experiments. When the CBI observations are used in combination with those from COBE -DMR, we find evidence for a flat universe, Ω tot = 1.00 (1 σ), a power-law index of primordial fluctuations, n s = 1.08 , and densities in cold dark matter, Ω cdm h 2 = 0.16 , and baryons, Ω b h 2 = 0.023 . With the addition of large-scale structure priors the Ω cdm h 2 value is sharpened to 0.10 , and we find Ω Λ = 0.67 . In the l < 1000 overlap region with the BOOMERANG, DASI, MAXIMA, and VSA experiments, the agreement between these four experiments is excellent, and we construct optimal power spectra in the CBI bands that demonstrate this agreement. We derive cosmological parameters for the combined cosmic microwave background (CMB) experiments and show that these parameter determinations are stable as we progress from the weak priors using only CMB observations and very broad restrictions on cosmic parameters, through the addition of information from large-scale structure surveys, Hubble parameter determinations, and Type Ia supernova results. The combination of these with CMB observations gives a vacuum energy estimate of Ω Λ = 0.70 , a Hubble parameter of h = 0.69 ± 0.04, and a cosmological age of 13.7 ± 0.2 Gyr. As the observations are pushed to higher multipoles, no anomalies relative to standard models appear, and extremely good consistency is found between the cosmological parameters derived for the CBI observations over the range 610 < l < 2000 and observations at lower l .