SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: SKY MAPS, SYSTEMATIC ERRORS, AND BASIC RESULTS

By N. Jarosik, C. Bennett, J. Dunkley, B. Gold, M. Greason, Mark Halpern, R. Hill, Gary F. Hinshaw, Alan Kogut, E. Komatsu and 12 more. 2010

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New full-sky temperature and polarization maps based on seven years of data from WMAP are presented. The new results are consistent with previous results, but have improved due to reduced noise from the additional integration time, improved knowledge of the instrument performance, and improved data analysis procedures. The improvements are described in detail. The seven-year data set is well fit by a minimal six-parameter flat ΛCDM model. The parameters for this model, using the WMAP data in conjunction with baryon acoustic oscillation data from the Sloan Digital Sky Survey and priors on H0 from Hubble Space Telescope observations, are Ωbh2 = 0.02260 ± 0.00053, Ωch2 = 0.1123 ± 0.0035, ΩΛ = 0.728+0.015−0.016, ns = 0.963 ± 0.012, τ = 0.087 ± 0.014, and σ8 = 0.809 ± 0.024 (68% CL uncertainties). The temperature power spectrum signal-to-noise ratio per multipole is greater that unity for multipoles ℓ ≲ 919, allowing a robust measurement of the third acoustic peak. This measurement results in improved constraints on the matter density, Ωmh2 = 0.1334+0.0056−0.0055, and the epoch of matter–radiation equality, zeq = 3196+134−133, using WMAP data alone. The new WMAP data, when combined with smaller angular scale microwave background anisotropy data, result in a 3σ detection of the abundance of primordial helium, YHe = 0.326 ± 0.075. When combined with additional external data sets, the WMAP data also yield better determinations of the total mass of neutrinos, ∑mν ⩽ 0.58 eV(95%CL), and the effective number of neutrino species, Neff = 4.34+0.86−0.88. The power-law index of the primordial power spectrum is now determined to be ns = 0.963 ± 0.012, excluding the Harrison–Zel'dovich–Peebles spectrum by >3σ. These new WMAP measurements provide important tests of big bang cosmology.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3596a3ecb1076ada17526cbeaa3e8546f60134d7

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Citations in the corpus

THE MASS SPECTRUM OF THE FIRST STARS (2014, methodology): “Throughout this paper we assume the Λ cold dark matter universe with cosmological parameters of Ωb = 0.049, Ω0 = 0.27, ΩΛ = 0.73, and h = 0.71, based on seven-year WMAP results (Komatsu et al. 2011; Jarosik et al. 2011).”
The Atacama Cosmology Telescope: temperature and gravitational lensing power spectrum measurements from three seasons of data (2013, methodology): “Comparison of a sky patch from the WMAP 7-year 94 GHz map [22] (top) with the map of the same region made from ACT 148GHz (bottom) observations (co-added across seasons).”
SEMI-ANALYTIC GALAXY EVOLUTION (SAGE): MODEL CALIBRATION AND BASIC RESULTS (2016, result): “The chosen cosmological parameters were very close to those of the WMAP7 data (Jarosik et al. 2011), while maintaining consistency with WMAP5 (Dunkley et al. 2009; also see Komatsu et al. 2009).”
GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, methodology): “…2011 November 20 Trujillo-Gomez et al. (A color version of this figure is available in the online journal.) with the WMAP seven-year data (WMAP7; Jarosik et al. 2011) and with WMAP5 combined with Baryon Acoustic Oscillations and Type 1a Supernova data (Hinshaw et al. 2009; Komatsu et al. 2009;…”
Dirac equation for cold atoms in artificial curved spacetimes (2010, background): “The propagation of fermions in curved space is not experimentally accessible in highenergy physics/cosmology as the (piece of the) Universe that we are nowadays able to probe is practically flat [78].”
DEPENDENCE OF THE OUTER DENSITY PROFILES OF HALOS ON THEIR MASS ACCRETION RATE (2014, background): “…parameters are compatible with constraints from a combination of WMAP5, Baryon Acoustic Oscillations and Type Ia Supernovae (Komatsu et al. 2011; Jarosik et al. 2011), X-Ray cluster abundance evolution (Vikhlinin et al. 2009), and observations of the clustering of galaxies and…”
Dark Matter: A Primer (2010, methodology): “18 N. Jarosik et al. “Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP1) Observations: Sky Maps, Systematic Errors, and Basic Results,” arXiv:1001.4744v1 (2010).”
Planck 2015 results. I. Overview of products and scientific results (2015, methodology): “5.4.1, the WMAP5 Solar dipole was underestimated by 0.28 % when compared with the Planck best-measured amplitude, leading to an under-calibration of 0.28 % in the Planck 2013 maps.”
Local gravity versus local velocity: solutions for β and non-linear bias (2010, methodology): “Taking σ 8g = 0.97 ± 0.05 (Westover 2007; Reid et al. 2010) yields σ 8 = σ 8g/b = 0.65 ± 0.11 for the underlying mass density field, marginally consistent with the latest Wilkinson Microwave Anisotropy Probe (WMAP) results (Larson et al. 2011) of σ 8 = 0.8 ± 0.03 (see also Jarosik et al. (2010)).”
Subhaloes going Notts: the subhalo‐finder comparison project (2012, result): “These parameters are consistent with the latest WMAP data (Jarosik et al. 2011) althoughσ8 is a little high.”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: FINAL MAPS AND RESULTS (2012, methodology): “The K−Q band brightness variations were previously presented for the seven-year data in Jarosik et al. (2011), where they were described as variations in the WMAP calibration.”