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Title:
Nine-year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Final Maps and Results
Authors:
Bennett, C. L.; Larson, D.; Weiland, J. L.; Jarosik, N.; Hinshaw, G.; Odegard, N.; Smith, K. M.; Hill, R. S.; Gold, B.; Halpern, M.; Komatsu, E.; Nolta, M. R.; Page, L.; Spergel, D. N.; Wollack, E.; Dunkley, J.; Kogut, A.; Limon, M.; Meyer, S. S.; Tucker, G. S.; Wright, E. L.
Affiliation:
AA(Department of Physics & Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218-2686, USA ), AB(Department of Physics & Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218-2686, USA), AC(Department of Physics & Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218-2686, USA), AD(Department of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544-0708, USA), AE(Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, Canada), AF(ADNET Systems, Inc., 7515 Mission Drive, Suite A100, Lanham, MD 20706, USA), AG(Perimeter Institute for Theoretical Physics, Waterloo, ON N2L 2Y5, Canada ; Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544-1001, USA), AH(ADNET Systems, Inc., 7515 Mission Drive, Suite A100, Lanham, MD 20706, USA), AI(School of Physics & Astronomy, University of Minnesota, 116 Church Street S.E., Minneapolis, MN 55455, USA), AJ(Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, Canada), AK(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild Str. 1, D-85741 Garching, Germany ; Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), Todai Institutes for Advanced Study, University of Tokyo, Kashiwa 277-8583, Japan ; Texas Cosmology Center and Department of Astronomy, University of Texas, Austin, 2511 Speedway, RLM 15.306, Austin, TX 78712, USA), AL(Canadian Institute for Theoretical Astrophysics, 60 St. George Street, University of Toronto, Toronto, ON M5S 3H8, Canada), AM(Department of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544-0708, USA), AN(Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544-1001, USA ; Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), Todai Institutes for Advanced Study, University of Tokyo, Kashiwa 277-8583, Japan), AO(Code 665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA), AP(Oxford Astrophysics, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK), AQ(Code 665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA), AR(Columbia Astrophysics Laboratory, 550 West 120th Street, Mail Code 5247, New York, NY 10027-6902, USA), AS(Departments of Astrophysics and Physics, KICP and EFI, University of Chicago, Chicago, IL 60637, USA), AT(Department of Physics, Brown University, 182 Hope Street, Providence, RI 02912-1843, USA), AU(UCLA Physics & Astronomy, P.O. Box 951547, Los Angeles, CA 90095-1547, USA)
Publication:
The Astrophysical Journal Supplement, Volume 208, Issue 2, article id. 20, 54 pp. (2013). (ApJS Homepage)
Publication Date:
10/2013
Origin:
IOP
Astronomy Keywords:
cosmic background radiation, cosmology: observations, dark matter, early universe, instrumentation: detectors, space vehicles, space vehicles: instruments, telescopes
DOI:
10.1088/0067-0049/208/2/20
Bibliographic Code:
2013ApJS..208...20B

Abstract

We present the final nine-year maps and basic results from the Wilkinson Microwave Anisotropy Probe (WMAP) mission. The full nine-year analysis of the time-ordered data provides updated characterizations and calibrations of the experiment. We also provide new nine-year full sky temperature maps that were processed to reduce the asymmetry of the effective beams. Temperature and polarization sky maps are examined to separate cosmic microwave background (CMB) anisotropy from foreground emission, and both types of signals are analyzed in detail. We provide new point source catalogs as well as new diffuse and point source foreground masks. An updated template-removal process is used for cosmological analysis; new foreground fits are performed, and new foreground-reduced CMB maps are presented. We now implement an optimal C -1 weighting to compute the temperature angular power spectrum. The WMAP mission has resulted in a highly constrained LambdaCDM cosmological model with precise and accurate parameters in agreement with a host of other cosmological measurements. When WMAP data are combined with finer scale CMB, baryon acoustic oscillation, and Hubble constant measurements, we find that big bang nucleosynthesis is well supported and there is no compelling evidence for a non-standard number of neutrino species (N eff = 3.84 ± 0.40). The model fit also implies that the age of the universe is t 0 = 13.772 ± 0.059 Gyr, and the fit Hubble constant is H 0 = 69.32 ± 0.80 km s-1 Mpc-1. Inflation is also supported: the fluctuations are adiabatic, with Gaussian random phases; the detection of a deviation of the scalar spectral index from unity, reported earlier by the WMAP team, now has high statistical significance (ns = 0.9608 ± 0.0080); and the universe is close to flat/Euclidean (\Omega _k = -0.0027^{+ 0.0039}_{-0.0038}). Overall, the WMAP mission has resulted in a reduction of the cosmological parameter volume by a factor of 68,000 for the standard six-parameter LambdaCDM model, based on CMB data alone. For a model including tensors, the allowed seven-parameter volume has been reduced by a factor 117,000. Other cosmological observations are in accord with the CMB predictions, and the combined data reduces the cosmological parameter volume even further. With no significant anomalies and an adequate goodness of fit, the inflationary flat LambdaCDM model and its precise and accurate parameters rooted in WMAP data stands as the standard model of cosmology.

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