Статья

FIVE-YEAR<i>WILKINSON MICROWAVE ANISOTROPY PROBE</i>OBSERVATIONS: COSMOLOGICAL INTERPRETATION

Eiichiro KomatsuDepartment of Astronomy, University of Texas, Austin, 2511 Speedway, RLM 15.306, Austin, TX 78712, USAJ. DunkleyDepartment of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544-0708, USAMichael R. NoltaCanadian Institute for Theoretical Astrophysics, 60 St. George St, University of Toronto, Toronto, ON M5S 3H8, CanadaC. L. BennettDepartment of Physics and Astronomy, The Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218-2686, USAB. GoldDepartment of Physics and Astronomy, The Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218-2686, USAG. HinshawCode 665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USAN. JarosikDepartment of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544-0708, USAD. LarsonDepartment of Physics and Astronomy, The Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218-2686, USAM. LimonColumbia Astrophysics Laboratory, 550 W. 120th St., Mail Code 5247, New York, NY 10027-6902, USALyman A. PageDepartment of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544-0708, USADavid N. SpergelDepartment of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544-1001, USAM. HalpernDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, CanadaRobert HillAdnet Systems, Inc., 7515 Mission Dr., Suite A100, Lanham, MD 20706, USAA. KogutCode 665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USAS. S. MeyerDepartments of Astrophysics and Physics, KICP and EFI, University of Chicago, Chicago, IL 60637, USAGregory S. TuckerDepartment of Physics, Brown University, 182 Hope St., Providence, RI 02912-1843, USAJ. L. WeilandAdnet Systems, Inc., 7515 Mission Dr., Suite A100, Lanham, MD 20706, USAEdward J. WollackCode 665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USAE. L. Wright

2009en

ABI

Аннотация

(Abridged) The WMAP 5-year data strongly limit deviations from the minimal LCDM model. We constrain the physics of inflation via Gaussianity, adiabaticity, the power spectrum shape, gravitational waves, and spatial curvature. We also constrain the properties of dark energy, parity-violation, and neutrinos. We detect no convincing deviations from the minimal model. The parameters of the LCDM model, derived from WMAP combined with the distance measurements from the Type Ia supernovae (SN) and the Baryon Acoustic Oscillations (BAO), are: Omega_b=0.0456+-0.0015, Omega_c=0.228+-0.013, Omega_Lambda=0.726+-0.015, H_0=70.5+-1.3 km/s/Mpc, n_s=0.960+-0.013, tau=0.084+-0.016, and sigma_8=0.812+-0.026. With WMAP+BAO+SN, we find the tensor-to-scalar ratio r<0.22 (95% CL), and n_s>1 is disfavored regardless of r. We obtain tight, simultaneous limits on the (constant) equation of state of dark energy and curvature. We provide a set of "WMAP distance priors," to test a variety of dark energy models. We test a time-dependent w with a present value constrained as -0.33<1+w_0<0.21 (95% CL). Temperature and matter fluctuations obey the adiabatic relation to within 8.9% and 2.1% for the axion and curvaton-type dark matter, respectively. The TE and EB spectra constrain cosmic parity-violation. We find the limit on the total mass of neutrinos, sum(m_nu)<0.67 eV (95% CL), which is free from the uncertainty in the normalization of the large-scale structure data. The effective number of neutrino species is constrained as N_{eff} = 4.4+-1.5 (68%), consistent with the standard value of 3.04. Finally, limits on primordial non-Gaussianity are -9<f_{NL}^{local}<111 and -151<f_{NL}^{equil}<253 (95% CL) for the local and equilateral models, respectively.

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Идентификаторы

DOI: 10.1088/0067-0049/180/2/330

Цитирования и источники

Цитирований: 5Использованных источников: 0

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