Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:0803.0732)
· References in the article
· Citations to the Article (1395) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Five-Year Wilkinson Microwave Anisotropy Probe Observations: Data Processing, Sky Maps, and Basic Results
Authors:
Hinshaw, G.; Weiland, J. L.; Hill, R. S.; Odegard, N.; Larson, D.; Bennett, C. L.; Dunkley, J.; Gold, B.; Greason, M. R.; Jarosik, N.; Komatsu, E.; Nolta, M. R.; Page, L.; Spergel, D. N.; Wollack, E.; Halpern, M.; Kogut, A.; Limon, M.; Meyer, S. S.; Tucker, G. S.; Wright, E. L.
Affiliation:
AA(Code 665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA ), AB(Adnet Systems, Inc., 7515 Mission Dr., Suite A100, Lanham, MD 20706, USA), AC(Adnet Systems, Inc., 7515 Mission Dr., Suite A100, Lanham, MD 20706, USA), AD(Adnet Systems, Inc., 7515 Mission Dr., Suite A100, Lanham, MD 20706, USA), AE(Department of Physics and Astronomy, The Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218-2686, USA), AF(Department of Physics and Astronomy, The Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218-2686, USA), AG(Department of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544-0708, USA; Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544-1001, USA; Astrophysics, University of Oxford, Keble Road, Oxford, OX1 3RH, UK), AH(Department of Physics and Astronomy, The Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218-2686, USA), AI(Adnet Systems, Inc., 7515 Mission Dr., Suite A100, Lanham, MD 20706, USA), AJ(Department of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544-0708, USA), AK(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 St, 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; Princeton Center for Theoretical Physics, Princeton University, Princeton, NJ 08544, USA), AO(Code 665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA), AP(Department of Physics and Astronomy, University of British Columbia, Vancouver BC V6T 1Z1, Canada), AQ(Code 665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA), AR(Columbia Astrophysics Laboratory, 550 W. 120th St., 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 St., Providence, RI 02912-1843, USA), AU(UCLA Physics and Astronomy, P.O. Box 951547, Los Angeles, CA 90095-1547, USA)
Publication:
The Astrophysical Journal Supplement, Volume 180, Issue 2, pp. 225-245 (2009). (ApJS Homepage)
Publication Date:
02/2009
Origin:
IOP
Astronomy Keywords:
cosmic microwave background, cosmology: observations, early universe, dark matter, space vehicles, space vehicles: instruments, instrumentation: detectors, telescopes
DOI:
10.1088/0067-0049/180/2/225
Bibliographic Code:
2009ApJS..180..225H

Abstract

We present new full-sky temperature and polarization maps in five frequency bands from 23 to 94 GHz, based on data from the first five years of the Wilkinson Microwave Anisotropy Probe (WMAP) sky survey. The new maps are consistent with previous maps and are more sensitive. The five-year maps incorporate several improvements in data processing made possible by the additional years of data and by a more complete analysis of the instrument calibration and in-flight beam response. We present several new tests for systematic errors in the polarization data and conclude that W-band polarization data is not yet suitable for cosmological studies, but we suggest directions for further study. We do find that Ka-band data is suitable for use; in conjunction with the additional years of data, the addition of Ka band to the previously used Q- and V-band channels significantly reduces the uncertainty in the optical depth parameter, tau. Further scientific results from the five-year data analysis are presented in six companion papers and are summarized in Section 7 of this paper. With the five-year WMAP data, we detect no convincing deviations from the minimal six-parameter LambdaCDM model: a flat universe dominated by a cosmological constant, with adiabatic and nearly scale-invariant Gaussian fluctuations. Using WMAP data combined with measurements of Type Ia supernovae and Baryon Acoustic Oscillations in the galaxy distribution, we find (68% CL uncertainties): Omega b h 2 = 0.02267+0.00058 -0.00059, Omega c h 2 = 0.1131 ± 0.0034, OmegaLambda = 0.726 ± 0.015, ns = 0.960 ± 0.013, tau = 0.084 ± 0.016, and Delta_{R}^2 = (2.445± 0.096)× 10^{-9} at k = 0.002 Mpc-1. From these we derive sigma8 = 0.812 ± 0.026, H 0 = 70.5 ± 1.3 km s-1 Mpc-1, Omega b = 0.0456 ± 0.0015, Omega c = 0.228 ± 0.013, Omega m h 2 = 0.1358+0.0037 -0.0036, z reion = 10.9 ± 1.4, and t 0 = 13.72 ± 0.12 Gyr. The new limit on the tensor-to-scalar ratio is r < 0.22(95%CL), while the evidence for a running spectral index is insignificant, dns /dln k = -0.028 ± 0.020 (68% CL). We obtain tight, simultaneous limits on the (constant) dark energy equation of state and the spatial curvature of the universe: -0.14 < 1 + w < 0.12(95%CL) and -0.0179 < Omega k < 0.0081(95%CL). The number of relativistic degrees of freedom, expressed in units of the effective number of neutrino species, is found to be N eff = 4.4 ± 1.5 (68% CL), consistent with the standard value of 3.04. Models with N eff = 0 are disfavored at >99.5% confidence. Finally, new limits on physically motivated primordial non-Gaussianity parameters are -9 < f local NL < 111 (95% CL) and -151 < f equil NL < 253 (95% CL) for the local and equilateral models, respectively.

WMAP is the result of a partnership between Princeton University and NASA's Goddard Space Flight Center. Scientific guidance is provided by the WMAP Science Team.

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints