Wilkinson Microwave Anisotropy Probe (WMAP) Three Year Results: Implications for Cosmology Export

@misc{citeulike:557220, abstract = {A simple cosmological model with only six parameters (matter density, Omega\_m h^2, baryon density, Omega\_b h^2, Hubble Constant, H\_0, amplitude of fluctuations, sigma\_8, optical depth, tau, and a slope for the scalar perturbation spectrum, n\_s) fits not only the three year WMAP temperature and polarization data, but also small scale CMB data, light element abundances, large-scale structure observations, and the supernova luminosity/distance relationship. Using WMAP data only, the best fit values for cosmological parameters for the power-law flat LCDM model are (Omega\_m h^2, Omega\_b h^2, h, n\_s, tau, sigma\_8) = (0.127+0.007-0.013, 0.0223+0.0007-0.0009, 0.73 +- 0.03, 0.951+0.015-0.019, 0.09 +- 0.03, 0.74+0.05-0.06). The three year data dramatically shrink the allowed volume in this six-dimensional parameter space. Assuming that the primordial fluctuations are adiabatic with a power law spectrum, the WMAP data\_alone\_ require dark matter, and a spectral index that is significantly less than the Harrison-Zel'dovich-Peebles scale-invariant spectrum (n\_s=1,r=0). Models that suppress large-scale power through a running spectral index or a large-scale cut-off in the power spectrum are a slightly better fit to the WMAP and small scale CMB data than the power-law LCDM model (Delta chi^2 = 3) The combination of WMAP and other astronomical data yields significant constraints on the geometry of the universe, the equation of state of the dark energy, the gravitational wave energy density, and neutrino properties. Consistent with the predictions of simple inflationary theories, we detect no significant deviations from Gaussianity in the CMB maps.}, archivePrefix = {arXiv}, author = {Spergel, D. N. and Bean, R. and Dore', O. and Nolta, M. R. and Bennett, C. L. and Hinshaw, G. and Jarosik, N. and Komatsu, E. and Page, L. and Peiris, H. V. and Verde, L. and Barnes, C. and Halpern, M. and Hill, R. S. and Kogut, A. and Limon, M. and Meyer, S. S. and Odegard, N. and Tucker, G. S. and Weiland, J. L. and Wollack, E. and Wright, E. L.}, citeulike-article-id = {557220}, citeulike-linkout-0 = {http://arxiv.org/abs/astro-ph/0603449}, citeulike-linkout-1 = {http://arxiv.org/pdf/astro-ph/0603449}, day = {19}, eprint = {astro-ph/0603449}, keywords = {constraints, cosmology, inflation, wmap}, month = {Mar}, posted-at = {2006-09-26 11:20:55}, priority = {2}, title = {Wilkinson Microwave Anisotropy Probe (WMAP) Three Year Results: Implications for Cosmology}, url = {http://arxiv.org/abs/astro-ph/0603449}, year = {2006} }

TY - ELEC ID - citeulike:557220 L3 - citeulike-article-id:557220 N2 - A simple cosmological model with only six parameters (matter density, Omega_m h^2, baryon density, Omega_b h^2, Hubble Constant, H_0, amplitude of fluctuations, sigma_8, optical depth, tau, and a slope for the scalar perturbation spectrum, n_s) fits not only the three year WMAP temperature and polarization data, but also small scale CMB data, light element abundances, large-scale structure observations, and the supernova luminosity/distance relationship. Using WMAP data only, the best fit values for cosmological parameters for the power-law flat LCDM model are (Omega_m h^2, Omega_b h^2, h, n_s, tau, sigma_8) = (0.127+0.007-0.013, 0.0223+0.0007-0.0009, 0.73 +- 0.03, 0.951+0.015-0.019, 0.09 +- 0.03, 0.74+0.05-0.06). The three year data dramatically shrink the allowed volume in this six-dimensional parameter space. Assuming that the primordial fluctuations are adiabatic with a power law spectrum, the WMAP data_alone_ require dark matter, and a spectral index that is significantly less than the Harrison-Zel'dovich-Peebles scale-invariant spectrum (n_s=1,r=0). Models that suppress large-scale power through a running spectral index or a large-scale cut-off in the power spectrum are a slightly better fit to the WMAP and small scale CMB data than the power-law LCDM model (Delta chi^2 = 3) The combination of WMAP and other astronomical data yields significant constraints on the geometry of the universe, the equation of state of the dark energy, the gravitational wave energy density, and neutrino properties. Consistent with the predictions of simple inflationary theories, we detect no significant deviations from Gaussianity in the CMB maps. TI - Wilkinson Microwave Anisotropy Probe (WMAP) Three Year Results: Implications for Cosmology KW - constraints KW - cosmology KW - inflation KW - wmap AU - Spergel, DN AU - Bean, R AU - Dore', O AU - Nolta, MR AU - Bennett, CL AU - Hinshaw, G AU - Jarosik, N AU - Komatsu, E AU - Page, L AU - Peiris, HV AU - Verde, L AU - Barnes, C AU - Halpern, M AU - Hill, RS AU - Kogut, A AU - Limon, M AU - Meyer, SS AU - Odegard, N AU - Tucker, GS AU - Weiland, JL AU - Wollack, E AU - Wright, EL PY - 2006/Mar/19/ UR - http://arxiv.org/abs/astro-ph/0603449 ER -