Cosmological Parameters from the 2003 Flight of BOOMERANG

By C. MacTavish, P. Ade, J. Bock, J. Richard Bond, J. Borrill, A. Boscaleri, P. Cabella, C. Contaldi, B. Crill, P. Bernardis and 28 more. 2005

190 citations recorded by the source corpus.

We present the cosmological parameters from the CMB intensity and polarization power spectra of the 2003 Antarctic flight of the BOOMERANG telescope. The BOOMERANG data alone constrain the parameters of the ΛCDM model remarkably well and are consistent with constraints from a multiexperiment combined CMB data set. We add LSS data from the 2dF and SDSS redshift surveys to the combined CMB data set and test several extensions to the standard model including running of the spectral index, curvature, tensor modes, the effect of massive neutrinos, and an effective equation of state for dark energy. We also include an analysis of constraints to a model that allows a CDM isocurvature admixture.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering

View Paper: https://www.semanticscholar.org/paper/55d9b0229e95dc2ce08edebb1d6fff05683d287f

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Citations in the corpus

Inflating in a Better Racetrack (2006, background): “We also need to have the spectrum to be sufficiently flat,ns = 0.95 ± 0 .0 2 [36].”
CMB-S4 Science Case, Reference Design, and Project Plan (2019, background): “[56, 57, 58, 59, 34, 31]) at the roughly 1% level, depending on precise assumptions made about the spectral shape and multi-mode admixtures of isocurvature.”
The Atacama Cosmology Telescope: CMB polarization at 200 < ℓ < 9000 (2014, unknown): “For example, primordial isocurva-ture perturbations alter the phase of the oscillations in polarization relative to temperature compared to pure adiabatic perturbations (e.g., Bond & Efstathiou 1987; Bucher et al. 2004; MacTavish et al. 2006; Sievers et al. 2007).”
The Halo Mass Function: High-Redshift Evolution and Universality (2007, background): “…1:0; CDM ¼ 0:253; baryon ¼ 0:048; 8 ¼ 0:9; H0 ¼ 70 km s 1 Mpc 1; n ¼ 1; ð18Þ in concordancewith cosmicmicrowave background and large-scale structure observations (MacTavish et al. 2006) (the third-year Wilkinson Microwave Anisotropy Probe observations suggest a lower value of 8; Spergel et al.…”
Revisiting Bimaximal Neutrino Mixing in a Model with S(4) Discrete Symmetry (2009, methodology): “60 eV corresponds to the combination of the Cosmic Microwave Background (CMB) anisotropy data (from WMAP 5y [24], Arcminute Cosmology Bolometer Array Receiver (ACBAR) [25], Very Small Array (VSA) [26], Cosmic Background Imager (CBI) [27] and BOOMERANG [28] experiments) plus the large-scale structure”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, background): “…spectrum data, the constraints on cosmological parameters can be tightened, through the breaking of certain degeneracies (Efstathiou et al. 2002; Percival et al. 2002; Spergel et al. 2003; Tegmark et al. 2004b; Seljak et al. 2005; MacTavish et al. 2006; Sanchez et al. 2006; Spergel et al. 2006).”