SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP ) OBSERVATIONS: SKY MAPS, SYSTEMATIC ERRORS, AND BASIC RESULTS
- Department of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544-0708 (United States)
- Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218-2686 (United States)
- Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH (United Kingdom)
- ADNET Systems, Inc., 7515 Mission Dr., Suite A100 Lanham, MD 20706 (United States)
- Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1 (Canada)
- Code 665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771 (United States)
- Department of Astronomy, University of Texas, Austin, 2511 Speedway, RLM 15.306, Austin, TX 78712 (United States)
- Columbia Astrophysics Laboratory, 550 West 120th Street, Mail Code 5247, New York, NY 10027-6902 (United States)
- Departments of Astrophysics and Physics, KICP and EFI, University of Chicago, Chicago, IL 60637 (United States)
- Canadian Institute for Theoretical Astrophysics, 60 St. George Street, University of Toronto, Toronto, ON M5S 3H8 (Canada)
- Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544-1001 (United States)
- Department of Physics, Brown University, 182 Hope St., Providence, RI 02912-1843 (United States)
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 {Lambda}CDM 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 H{sub 0} from Hubble Space Telescope observations, are {Omega}{sub b} h {sup 2} = 0.02260 {+-} 0.00053, {Omega}{sub c} h {sup 2} = 0.1123 {+-} 0.0035, {Omega}{sub {Lambda}} = 0.728{sup +0.015}{sub -0.016}, n{sub s} = 0.963 {+-} 0.012, {tau} = 0.087 {+-} 0.014, and {sigma}{sub 8} = 0.809 {+-} 0.024 (68% CL uncertainties). The temperature power spectrum signal-to-noise ratio per multipole is greater that unity for multipoles l {approx}< 919, allowing a robust measurement of the third acoustic peak. This measurement results in improved constraints on the matter density, {Omega}{sub m} h {sup 2} = 0.1334{sup +0.0056}{sub -0.0055}, and the epoch of matter-radiation equality, z{sub eq} = 3196{sup +134}{sub -133}, using WMAP data alone. The new WMAP data, when combined with smaller angular scale microwave background anisotropy data, result in a 3{sigma} detection of the abundance of primordial helium, Y{sub He} = 0.326 {+-} 0.075. When combined with additional external data sets, the WMAP data also yield better determinations of the total mass of neutrinos, {Sigma}M{sub {nu}} {<=} 0.58 eV(95%CL), and the effective number of neutrino species, N{sub eff} = 4.34{sup +0.86}{sub -0.88}. The power-law index of the primordial power spectrum is now determined to be n{sub s} = 0.963 {+-} 0.012, excluding the Harrison-Zel'dovich-Peebles spectrum by >3{sigma}. These new WMAP measurements provide important tests of big bang cosmology.
- OSTI ID:
- 21560532
- Journal Information:
- Astrophysical Journal, Supplement Series, Vol. 192, Issue 2; Other Information: DOI: 10.1088/0067-0049/192/2/14; ISSN 0067-0049
- Country of Publication:
- United States
- Language:
- English
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