A Measurement by BOOMERANG of Multiple Peaks in the Angular Power Spectrum of the Cosmic Microwave Background

By C. Netterfield, P. Ade, J. Bock, J. Richard Bond, J. Borrill, A. Boscaleri, K. Coble, C. Contaldi, B. Crill, P. Bernardis and 23 more. 2001

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This paper presents a measurement of the angular power spectrum of the cosmic microwave background from l = 75 to l = 1025 (~10' to 2.°4) from a combined analysis of four 150 GHz channels in the BOOMERANG experiment. The spectrum contains multiple peaks and minima, as predicted by standard adiabatic inflationary models in which the primordial plasma undergoes acoustic oscillations. These results, in concert with other types of cosmological measurements and theoretical models, significantly constrain the values of Ωtot, Ωbh2, Ωch2, and ns.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/4c8d2e460f864c80428c917a1f385c35b35077e7

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Citations in the corpus

The Cosmological Baryon Density from the Deuterium-to-Hydrogen Ratio in QSO Absorption Systems: D/H toward Q1243+3047 (2003, methodology): “%) that agrees with values from the anisotropy of the Cosmic Microwave Background: Ωbh 2 = 0.021±0.003 from the Netterfield et al. (2002) analysis of BOOMERANG data and Ωbh 2 = 0.022+0.004 −0.003 from the Pryke et al. (2002) analysis of the DASI results.”
Continuum and Emission-Line Strength Relations for a Large Active Galactic Nuclei Sample (2002, background): “Introducing ¼ 0:7 (Netterfield et al. 2002) instead of ¼ 0:0, the luminosities at the highest redshifts would be 10% smaller, while at low redshifts they would reach a maximum of 20% larger at redshift z ’ 1.”
The Detectability of the First Stars and Their Cluster Enrichment Signatures (2003, background): “The choice of these parameters is based mainly on measurements of cosmic microwave background anisotropies (e.g., Balbi et al. 2000; Netterfield et al. 2002; Pryke et al. 2002) and the abundance of galaxy clusters (e.g., Viana & Liddle 1996).”
Detection of polarization in the cosmic microwave background using DASI (2002, methodology): “…of temperature anisotropy was made on large angular scales by the COBE DMR instrument (Smoot et al. 1992) and recently there has been considerable progress in measuring the anisotropy on finer angular scales (Miller et al. 1999; Halverson et al. 2002; Netterfield et al. 2002; Lee et al. 2001).”
Cosmological Constraints from a Combination of Galaxy Clustering and Lensing -- III. Application to SDSS Data (2012, background): “…power spectrum of cosmic microwave background c© 2008 RAS (CMB) temperature fluctuations (e.g., Balbi et al. 2000; Lange et al. 2001; Pryke et al. 2002; Netterfield et al. 2002; Ruhl et al. 2003) combined with the results on the Hubble constant from the Hubble Key Project (Freedman et al.…”
Cosmological constraints from archeops (2002, background): “These results are in good agreement with recent analyses performed by other teams (Netterfield et al. 2002; Pryke et al. 2002; Rubino-Martin et al. 2002; Sievers et al. 2002; Wang et al. 2002).”
High-Resolution Observations of the Cosmic Microwave Background Power Spectrum with ACBAR (2002, methodology): “A number of experiments have characterized the power spectrum up to and including the third acoustic peak (Lee et al. 2001; Netterfield et al. 2002; Halverson et al. 2002).”