SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: POWER SPECTRA AND WMAP-DERIVED PARAMETERS

The WMAP mission has produced sky maps from seven years of observations at L2. We present the angular power spectra derived from the seven-year maps and discuss the cosmological conclusions that can be inferred from WMAP data alone. With the seven-year data, the temperature (TT) spectrum measurement has a signal-to-noise ratio per multipole that exceeds unity for l 2.7(95%CL). Also, using WMAP data alone, the primordial helium mass fraction is found to be Y He = 0.28+0.14 ?0.15, and with data from higher-resolution cosmic microwave background experiments included, we now establish the existence of pre-stellar helium at >3?. These new WMAP measurements provide important tests of big bang cosmology.

[1]  Roger Penrose,et al.  Note on the Bondi-Metzner-Sachs Group , 1966 .

[2]  F. Rohrlich,et al.  Spin‐s Spherical Harmonics and ð , 1967 .

[3]  Turner,et al.  CBR anisotropy and the running of the scalar spectral index. , 1995, Physical review. D, Particles and fields.

[4]  U. Seljak,et al.  A Line of sight integration approach to cosmic microwave background anisotropies , 1996, astro-ph/9603033.

[5]  U. Seljak,et al.  An all sky analysis of polarization in the microwave background , 1996, astro-ph/9609170.

[6]  Albert Stebbins,et al.  Statistics of cosmic microwave background polarization , 1997 .

[7]  U. Toronto,et al.  Estimating the power spectrum of the cosmic microwave background , 1997, astro-ph/9708203.

[8]  Sara Seager,et al.  How Exactly Did the Universe Become Neutral? , 1999, astro-ph/9912182.

[9]  A. Lewis,et al.  Efficient computation of CMB anisotropies in closed FRW models , 1999, astro-ph/9911177.

[10]  Sara Seager,et al.  A New Calculation of the Recombination Epoch , 1999 .

[11]  Uros Seljak,et al.  The Sunyaev-Zel'dovich angular power spectrum as a probe of cosmological parameters , 2002 .

[12]  R. Gruenwald,et al.  The Evolution of Helium and Hydrogen Ionization Corrections as H II Regions Age , 2001, astro-ph/0109071.

[13]  C. B. Netterfield,et al.  MASTER of the Cosmic Microwave Background Anisotropy Power Spectrum: A Fast Method for Statistical Analysis of Large and Complex Cosmic Microwave Background Data Sets , 2001, astro-ph/0105302.

[14]  M. Halpern,et al.  First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Tests of Gaussianity , 2003 .

[15]  Edward J. Wollack,et al.  First year Wilkinson Microwave Anisotropy Probe (WMAP) observations: Determination of cosmological parameters , 2003, astro-ph/0302209.

[16]  M. Halpern,et al.  First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: The Angular Power Spectrum , 2003, astro-ph/0302217.

[17]  M. Halpern,et al.  First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Parameter Estimation Methodology , 2003 .

[18]  Edward J. Wollack,et al.  First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Preliminary Maps and Basic Results , 2003, astro-ph/0302207.

[19]  C. H. Anderson,et al.  Application of Monte Carlo Algorithms to the Bayesian Analysis of the Cosmic Microwave Background , 2002, astro-ph/0209560.

[20]  Benjamin D. Wandelt,et al.  Global, Exact Cosmic Microwave Background Data Analysis Using Gibbs Sampling , 2004 .

[21]  K. Olive,et al.  A Realistic Determination of the Error on the Primordial Helium Abundance: Steps toward Nonparametric Nebular Helium Abundances , 2004, astro-ph/0405588.

[22]  H. K. Eriksen,et al.  Power Spectrum Estimation from High-Resolution Maps by Gibbs Sampling , 2004 .

[23]  T. Thuan,et al.  Systematic Effects and a New Determination of the Primordial Abundance of 4He and dY/dZ from Observations of Blue Compact Galaxies , 2003, astro-ph/0310421.

[24]  David J. C. MacKay,et al.  Information Theory, Inference, and Learning Algorithms , 2004, IEEE Transactions on Information Theory.

[25]  Yuhong Yang,et al.  Information Theory, Inference, and Learning Algorithms , 2005 .

[26]  K. Gorski,et al.  HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere , 2004, astro-ph/0409513.

[27]  H. K. Eriksen,et al.  Cosmological parameter constraints as derived from the Wilkinson Microwave Anisotropy Probe data via Gibbs sampling and the Blackwell-Rao estimator , 2005 .

[28]  Constraining neutrino masses by CMB experiments alone , 2004, astro-ph/0409768.

[29]  M. Halpern,et al.  Three-year Wilkinson Microwave Anisotropy Probe (WMAP) observations: temperature analysis , 2006 .

[30]  H. K. Eriksen,et al.  A re-analysis of the three-year WMAP temperature power spectrum and likelihood , 2006 .

[31]  Elena Pierpaoli,et al.  Constraining Isocurvature Initial Conditions with WMAP 3-year data , 2006 .

[32]  Masahiro Kawasaki,et al.  Primordial Helium Abundance: A Reanalysis of the Izotov-Thuan Spectroscopic Sample , 2006 .

[33]  Rajib Saha,et al.  A Reanalysis of the 3 Year Wilkinson Microwave Anisotropy Probe Temperature Power Spectrum and Likelihood , 2007 .

[34]  Edward J. Wollack,et al.  Three Year Wilkinson Microwave Anistropy Probe (WMAP) Observations: Polarization Analysis , 2006, astro-ph/0603450.

[35]  M. Peimbert,et al.  Revised Primordial Helium Abundance Based on New Atomic Data , 2007, astro-ph/0701580.

[36]  Primordial Nucleosynthesis in the Precision Cosmology Era , 2007, 0712.1100.

[37]  A. Lewis.  Cosmological parameters from WMAP 5-year temperature maps , 2008, 0804.3865.

[38]  M. Halpern,et al.  FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: LIKELIHOODS AND PARAMETERS FROM THE WMAP DATA , 2008, 0803.0586.

[39]  A. Moss,et al.  How well do we understand cosmological recombination , 2007, 0711.1357.

[40]  M. Halpern,et al.  Five-Year Wilkinson Microwave Anisotropy Probe (WMAP1) Observations: Galactic Foreground Emission , 2008 .

[41]  M. Halpern,et al.  THEMICROWAVE ANISOTROPY PROBE (MAP )1 MISSION , 2003 .

[42]  H. K. Eriksen,et al.  COSMIC MICROWAVE BACKGROUND LIKELIHOOD APPROXIMATION BY A GAUSSIANIZED BLACKWELL–RAO ESTIMATOR , 2008, 0809.4624.

[43]  Edward J. Wollack,et al.  FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE * OBSERVATIONS: COSMOLOGICAL INTERPRETATION , 2008, 0803.0547.

[44]  K. Gorski,et al.  A MARKOV CHAIN MONTE CARLO ALGORITHM FOR ANALYSIS OF LOW SIGNAL-TO-NOISE COSMIC MICROWAVE BACKGROUND DATA , 2008, 0807.0624.

[45]  Matter temperature during cosmological recombination , 2009, 0902.3438.

[46]  F. Finelli,et al.  New estimates of the CMB angular power spectra from the WMAP 5 year low-resolution data , 2009, 0904.0789.

[47]  M. Halpern,et al.  FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: GALACTIC FOREGROUND EMISSION , 2008, 0803.0715.

[48]  E. Leitch,et al.  IMPROVED MEASUREMENTS OF THE TEMPERATURE AND POLARIZATION OF THE COSMIC MICROWAVE BACKGROUND FROM QUaD , 2009, 0906.1003.

[49]  Stefano Casertano,et al.  A REDETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE FROM A DIFFERENTIAL DISTANCE LADDER , 2009, 0905.0695.

[50]  E. Pierpaoli,et al.  Estimates of unresolved point source contribution to WMAP 5 , 2010, 1001.3659.

[51]  M. Halpern,et al.  SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP *) OBSERVATIONS: SKY MAPS, SYSTEMATIC ERRORS, AND BASIC RESULTS , 2011 .

[52]  M. Halpern,et al.  SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP ) OBSERVATIONS: ARE THERE COSMIC MICROWAVE BACKGROUND ANOMALIES? , 2010, 1001.4758.

[53]  Edward J. Wollack,et al.  SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: PLANETS AND CELESTIAL CALIBRATION SOURCES , 2010, 1001.4731.

[54]  Edward J. Wollack,et al.  FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: COSMOLOGICAL INTERPRETATION , 2008, 0803.0547.