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Cited by 4,860Cosmology and Gravitation TheoriesDark Matter and Cosmic PhenomenaGalaxies: Formation, Evolution, Phenomena

First‐Year Wilkinson Microwave Anisotropy Probe ( WMAP ) Observations: Preliminary Maps and Basic Results

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Bennett, C. L., Halpern, M., Hinshaw, G., Jarosik, N., Kogut, A., Limon, M., Meyer, S. S., Page, L. +13 more·2003·The Astrophysical Journal Supplement Series
DOI 10.1086/377253
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Abstract

We present full sky microwave maps in five frequency bands (23 to 94 GHz) from the WMAP first year sky survey. Calibration errors are less than 0.5% and the low systematic error level is well specified. The cosmic microwave background (CMB) is separated from the foregrounds using multifrequency data. The sky maps are consistent with the 7 in. full-width at half-maximum (FWHM) Cosmic Background Explorer (COBE) maps. We report more precise, but consistent, dipole and quadrupole values. The CMB anisotropy obeys Gaussian statistics with -58 less than f(sub NL) less than 134 (95% CL). The 2 less than or = l less than or = 900 anisotropy power spectrum is cosmic variance limited for l less than 354 with a signal-to-noise ratio greater than 1 per mode to l = 658. The temperature-polarization cross-power spectrum reveals both acoustic features and a large angle correlation from reionization. The optical depth of reionization is tau = 0.17 +/- 0.04, which implies a reionization epoch of t(sub r) = 180(sup +220, sub -80) Myr (95% CL) after the Big Bang at a redshift of z(sub r) = 20(sup +10, sub -9) (95% CL) for a range of ionization scenarios. This early reionization is incompatible with the presence of a significant warm dark matter density. A best-fit cosmological model to the CMB and other measures of large scale structure works remarkably well with only a few parameters. The age of the best-fit universe is t(sub 0) = 13.7 +/- 0.2 Gyr old. Decoupling was t(sub dec) = 379(sup +8, sub -7)kyr after the Big Bang at a redshift of z(sub dec) = 1089 +/- 1. The thickness of the decoupling surface was Delta(sub z(sub dec)) = 195 +/- 2. The matter density of the universe is Omega(sub m)h(sup 2) = 0.135(sup +0.008, sub -0.009) the baryon density is Omega(sub b)h(sup 2) = 0.0224 +/- 0.0009, and the total mass-energy of the universe is Omega(sub tot) = 1.02 +/- 0.02. There is progressively less fluctuation power on smaller scales, from WMAP to fine scale CMB measurements to galaxies and finally to the Ly-alpha forest. This is accounted for with a running spectral index, significant at the approx. 2(sigma) level. The spectral index of scalar fluctuations is fit as n(sub s) = 0.93 +/-0.03 at wavenumber k(sub o) = 0.05/Mpc ((sub eff) approx. = 700), with a slope of dn(sub s)/d I(sub nk) = -0.031(sup + 0.016, sub -0.018) in the best-fit model.

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  • The baryon asymmetry ratio is the only free input parameter that enters in nucleosynthesis calculations of the primordial abundance of light elements.

    “This is the only free input parameter that enters in nucleosynthesis calculations of the primordial abundance of light elements[12, 13].”

    From Phase Transitions in the Early and Present Universe (2006) · cites this paper as [12]

    Section 9.1 (p. 33) lists the baryon-to-photon ratio, and Section 9.2 (p. 34) links baryon density to light-element abundance measurements and Big Bang nucleosynthesis. Neither passage says that this ratio is the only free input parameter in primordial-abundance calculations. (LLM, conf=0.82)

    Experimental — accuracy not yet measured

  • The standard (homogeneous) BBN scenario is in good agreement with observations.

    “This is in good agreement with observations [12, 13].”

    From Phase Transitions in the Early and Present Universe (2006) · cites this paper as [12]

  • These quark nuggets could contribute to the dark matter today or affect BBN.

    “These quark nuggets could contribute to the dark matter today [95] or affect BBN [12, 13].”

    From Phase Transitions in the Early and Present Universe (2006) · cites this paper as [12]

    The citation to this paper is attached to the claim that quark nuggets could affect BBN, not to the separate dark-matter claim. Section 9.2 (p. 34) compares WMAP’s baryon-density measurement with one from Big Bang nucleosynthesis, but does not discuss quark nuggets or their effects on BBN. Searches for quark nuggets, strange quark matter, and nucleosynthesis effects found no passage addressing that claim. (LLM, conf=0.76)

    Experimental — accuracy not yet measured

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Cites

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Research works printed but not linked: 14

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Authors
Bennett, C. L., Halpern, M., Hinshaw, G., Jarosik, N., Kogut, A., Limon, M., Meyer, S. S., Page, L., Spergel, D. N., Tucker, G. S., Wollack, E., Wright, E. L., Barnes, C., Greason, M. R., Hill, R. S., Komatsu, E., Nolta, M. R., Odegard, N., Peiris, H. V., Verde, L., & Weiland, J. L.
Affiliations
  • Goddard Space Flight Center (US)
  • University of British Columbia (CA)
  • Princeton University (US)
  • University of Chicago (US)
  • University of California, Los Angeles (US)
  • Science Systems and Applications (United States) (US)
ORCID
Venue
The Astrophysical Journal Supplement Series
Publisher
American Astronomical Society
Published
2003-09
Volume
148
Issue
1
Pages
1-27
ISSN
  • 0067-0049 (ISSN-L)
  • 1538-4365
DOI
10.1086/377253
OpenAlex
W2075884494
Cited by
4,860
References
99
Citations by year
2026: 73 · 2025: 109 · 2024: 115 · 2023: 115 · 2022: 90 · 2021: 100 · 2020: 122 · 2019: 115 · 2018: 119 · 2017: 90 · 2016: 143 · 2015: 101 · 2014: 132 · 2013: 171 · 2012: 185
FWCI
354.79
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal Supplement Series (publishedVersion)
  • arXiv (Cornell University) (acceptedVersion)
  • NASA STI Repository (National Aeronautics and Space Administration) (submittedVersion)
  • CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
  • UCL Discovery (University College London) (submittedVersion)
  • arXiv (Cornell University)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
  • Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Dark Matter and Cosmic Phenomena
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
Keywords
WMAP, cosmic microwave background anisotropies, reionization optical depth, cosmic reionization, matter density, baryon density, dark energy equation of state, dark energy, scalar spectral index, running of the spectral index, isocurvature modes, tensor-to-scalar ratio, inflation (cosmology), warm dark matter, acoustic features

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