First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications For Inflation

By Hiranya V. Peiris, E. Komatsu, L. Verde, David N. Spergel, C. Bennett, Mark Halpern, Gary F. Hinshaw, N. Jarosik, Alan Kogut, M. Limon and 4 more. 2003

992 citations recorded by the source corpus.

We confront predictions of inflationary scenarios with the Wilkinson Microwave Anisotropy Probe (WMAP) data, in combination with complementary small-scale cosmic microwave background (CMB) measurements and large-scale structure data. The WMAP detection of a large-angle anticorrelation in the temperature-polarization cross-power spectrum is the signature of adiabatic superhorizon fluctuations at the time of decoupling. The WMAP data are described by pure adiabatic fluctuations: we place an upper limit on a correlated cold dark matter (CDM) isocurvature component. Using WMAP constraints on the shape of the scalar power spectrum and the amplitude of gravity waves, we explore the parameter space of inflationary models that is consistent with the data. We place limits on inflationary models; for example, a minimally coupled λϕ4 is disfavored at more than 3 σ using WMAP data in combination with smaller scale CMB and large-scale structure survey data. The limits on the primordial parameters using WMAP data alone are ns(k0 = 0.002 Mpc-1) = 1.20, dns/d ln k = -0.077, A(k0 = 0.002 Mpc-1) = 0.71 (68% CL), and r(k0 = 0.002 Mpc-1) < 1.28 (95% CL).

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Oceanography

View Paper: https://www.semanticscholar.org/paper/6ba1b28878681b5b01d02225486ea1118dd1653f

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Citations in the corpus

A Measurement of the Polarization-Temperature Angular Cross-Power Spectrum of the Cosmic Microwave Background from the 2003 Flight of BOOMERANG (2005, methodology): “This, as previously detected by the WMAP experiment (Peiris et al. 2003), is consistent with the presence of superhorizon adiabatic fluctuations (Spergel & Zaldarriaga 1997) and does not support models based on active perturbations like topological defects (Turok 1996).”
The First Stars (2003, methodology): “The second model, the “running” spectral index (RSI) model, is suggested by the combined analysis of the WMAP data, the 2dF galaxy redshift survey, and Lyman-α forest observations (Spergel et al. 2003, Peiris et al. 2003).”
Towards inflation in string theory (2003, methodology): “There are still some question marks to be examined, such as the unexpectedly small anisotropy of CMB at large angles [20].”
Halo Substructure and the Power Spectrum (2002, methodology): “…of the Wilkinson Microwave Anisotropy Probe (WMAP) measurements of CMB anisotropy presented by Spergel et al. (2003; see also Verde et al. 2003; Peiris et al. 2003) returns a best-fit spectral index to a pure power law primordial spectrum of n = 0.99 ± 0.04 when only the WMAP data are…”
Cosmological parameters from cosmic microwave background measurements and the final 2dF Galaxy Redshift Survey power spectrum (2006, methodology): “Peiris et al. (2003) found that models with a spectral index varying slowly with wavenumber give slightly better fits to the WMAP data, particularly when combined with estimates of the power spectrum of the Lyman α forest.”
An alternative to the cosmological 'concordance model' (2003, background): “Indeed the WMAP team (Peiris et al. 2003) have already noted that the model fit can be significantly improved (particularly to the outliers at ` = 22, 40 and 200) by allowing for oscillations in the primordial spectrum (Adams, Cresswell & Easther 2001) such as might be induced by phase transitions…”