Large-Angular-Scale Anisotropy in the Cosmic Background Radiation

Large Angular Scale Anisotropy in Cosmic Microwave Background Induced by Cosmic Strings.

B. Allen,1 R. R. Caldwell,2 E. P. S. Shellard,2 A. Stebbins,3 and S. Veeraraghavan4 1Department of Physics, University of Wisconsin—Milwaukee, P.O. Box 413, Milwaukee, Wisconsin 53201 2University of Cambridge, Department of Applied Mathematics and Theoretical Physics, Silver Street, Cambridge CB3 9EW, United Kingdom 3NASAyFermilab Astrophysics Center, P.O. Box 500, Batavia, Illinois 60510 4Univ...

The Amplitude and Spectral Index of the Large Angular Scale Anisotropy in the Cosmic Microwave Background Radiation

In many cosmological models, the large angular scale anisotropy in the cosmic microwave background is parameterized by a spectral index, n, and a quadrupolar amplitude, Q. For a Peebles-Harrison-Zel’dovich spectrum, n = 1. Using data from the Far Infra-Red Survey (FIRS) and a new statistical measure, a contour plot of the likelihood for cosmological models for which −1 < n < 3 and 0 ≤ Q ≤ 50 μK...

Large-scale anisotropy of the cosmic background radiation in Friedmann universes.

Large Angular Scale Polarization of the Cosmic Microwave Background Radiation and the Feasibility of its Detection

In addition to its spectrum and temperature anisotropy, the 2.7 K Cosmic Microwave Background (CMB) is also expected to exhibit a low level of polarization. The spatial power spectrum of the polarization can provide details about the formation of structure in the universe as well as its ionization history. Here we calculate the magnitude of the CMB polarization in various cosmological scenarios...

Large-scale polarization of the cosmic microwave background radiation.

The anisotropy and polarization of the cosmic microwave background radiation (CMBR) induced by the scalar and tensor metric perturbations are computed in the long-wavelength limit. It is found that the large-scale polarization of CMBR induced by the decaying tensor mode can reach a few percents. This is different from the scalar or inflation-induced tensor mode, whereas the polarization is at l...