FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: COSMOLOGICAL INTERPRETATION

Journal Article · Sun Feb 15 00:00:00 EST 2009 · Astrophysical Journal, Supplement Series

DOI:https://doi.org/10.1088/0067-0049/180/2/330; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21269307

Komatsu, E ^[1]; Dunkley, J; Jarosik, N; Page, L ^[2]; Nolta, M R ^[3]; Bennett, C L; Gold, B; Larson, D ^[4]; Hinshaw, G; Kogut, A; Wollack, E ^[5]; Limon, M ^[6]; Spergel, D N ^[7]; Halpern, M ^[8]; Hill, R S; Weiland, J L ^[9]; Meyer, S S ^[10]; Tucker, G S ^[11]

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1. Department of Astronomy, University of Texas, Austin, 2511 Speedway, RLM 15.306, Austin, TX 78712 (United States)
2. Department of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544-0708 (United States)
3. Canadian Institute for Theoretical Astrophysics, 60 St. George St, University of Toronto, Toronto, ON M5S 3H8 (Canada)
4. Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218-2686 (United States)
5. Code 665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771 (United States)
6. Columbia Astrophysics Laboratory, 550 W. 120th St., Mail Code 5247, New York, NY 10027-6902 (United States)
7. Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544-1001 (United States)
8. Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1 (Canada)
9. Adnet Systems, Inc., 7515 Mission Dr., Suite A100, Lanham, MD 20706 (United States)
10. Departments of Astrophysics and Physics, KICP and EFI, University of Chicago, Chicago, IL 60637 (United States)
11. Department of Physics, Brown University, 182 Hope St., Providence, RI 02912-1843 (United States)

The Wilkinson Microwave Anisotropy Probe (WMAP) 5-year data provide stringent limits on deviations from the minimal, six-parameter {lambda} cold dark matter model. We report these limits and use them to constrain the physics of cosmic inflation via Gaussianity, adiabaticity, the power spectrum of primordial fluctuations, gravitational waves, and spatial curvature. We also constrain models of dark energy via its equation of state, parity-violating interaction, and neutrino properties, such as mass and the number of species. We detect no convincing deviations from the minimal model. The six parameters and the corresponding 68% uncertainties, derived from the WMAP data combined with the distance measurements from the Type Ia supernovae (SN) and the Baryon Acoustic Oscillations (BAO) in the distribution of galaxies, are: {omega} {sub b} h {sup 2} = 0.02267{sup +0.00058} {sub -0.00059}, {omega} {sub c} h {sup 2} = 0.1131 {+-} 0.0034, {omega}{sub {lambda}} = 0.726 {+-} 0.015, n{sub s} = 0.960 {+-} 0.013, {tau} = 0.084 {+-} 0.016, and {delta}{sub R}{sup 2} = (2.445{+-}0.096)x10{sup -9} at k = 0.002 Mpc{sup -1}. From these, we derive {sigma}{sub 8} = 0.812 {+-} 0.026, H {sub 0} = 70.5 {+-} 1.3 km s{sup -1} Mpc{sup -1}, {omega} {sub b} = 0.0456 {+-} 0.0015, {omega} {sub c} = 0.228 {+-} 0.013, {omega} {sub m} h {sup 2} = 0.1358{sup +0.0037} {sub -0.0036}, z {sub reion} = 10.9 {+-} 1.4, and t {sub 0} = 13.72 {+-} 0.12 Gyr. With the WMAP data combined with BAO and SN, we find the limit on the tensor-to-scalar ratio of r < 0.22(95%CL), and that n{sub s} > 1 is disfavored even when gravitational waves are included, which constrains the models of inflation that can produce significant gravitational waves, such as chaotic or power-law inflation models, or a blue spectrum, such as hybrid inflation models. We obtain tight, simultaneous limits on the (constant) equation of state of dark energy and the spatial curvature of the universe: -0.14 < 1 + w < 0.12(95%CL) and -0.0179 < {omega} {sub k} < 0.0081(95%CL). We provide a set of 'WMAP distance priors', to test a variety of dark energy models with spatial curvature. We test a time-dependent w with a present value constrained as -0.33 < 1 + w {sub 0} < 0.21 (95% CL). Temperature and dark matter fluctuations are found to obey the adiabatic relation to within 8.9% and 2.1% for the axion-type and curvaton-type dark matter, respectively. The power spectra of TB and EB correlations constrain a parity-violating interaction, which rotates the polarization angle and converts E to B. The polarization angle could not be rotated more than -5.{sup 0}9 < {delta}{alpha} < 2.{sup 0}4 (95% CL) between the decoupling and the present epoch. We find the limit on the total mass of massive neutrinos of {sigma}m {sub {nu}} < 0.67 eV(95%CL), which is free from the uncertainty in the normalization of the large-scale structure data. The number of relativistic degrees of freedom (dof), expressed in units of the effective number of neutrino species, is constrained as N {sub eff} = 4.4 {+-} 1.5 (68%), consistent with the standard value of 3.04. Finally, quantitative limits on physically-motivated primordial non-Gaussianity parameters are -9 < f {sup local} {sub NL} < 111 (95% CL) and -151 < f {sup equil} {sub NL} < 253 (95% CL) for the local and equilateral models, respectively.

• OSTI ID: 21269307
• Journal Information: Astrophysical Journal, Supplement Series, Vol. 180, Issue 2; Other Information: DOI: 10.1088/0067-0049/180/2/330; Country of input: International Atomic Energy Agency (IAEA); ISSN 0067-0049
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
99 GENERAL AND MISCELLANEOUS//MATHEMATICS, COMPUTING, AND INFORMATION SCIENCE
ANISOTROPY
AXIONS
CHAOS THEORY
CORRELATIONS
COSMOLOGY
DEGREES OF FREEDOM
DISTANCE
EQUATIONS OF STATE
GALAXIES
GRAVITATIONAL WAVES
INFLATIONARY UNIVERSE
NEUTRINOS
NONLUMINOUS MATTER
PARITY
POLARIZATION
RELATIVISTIC RANGE
RELICT RADIATION
SPACE VEHICLES
TIME DEPENDENCE
UNIVERSE